The document summarizes the results of a stellar photometry study of the polar ring galaxy NGC 660 using archival Hubble Space Telescope images. Over 550 stars were resolved, including many blue and red supergiants belonging to the polar ring. Analysis of the color-magnitude diagram for polar ring stars showed they are best represented by isochrones with a metallicity of Z=0.008. Star formation in the polar ring appears to have been continuous, with the youngest detected stars having an age of about 7 million years.
Detection of the_central_star_of_the_planetary_nebula_ngc6302Sérgio Sacani
This document reports on the first direct detection of the central star of the planetary nebula NGC 6302 using the Wide Field Camera 3 on the Hubble Space Telescope. Photometry of the central star was obtained in two narrowband filters, F469N and F673N, from which the reddening was estimated to be c=3.1, corresponding to AV=6.6 magnitudes of extinction. Comparison to evolutionary tracks suggests the central star has a temperature of around 200,000 K, luminosity of 2000 L☉, and the nebula is around 2,200 years old. The high extinction from dust in the nebula had previously prevented direct detection of the central star.
Stars and gas_in_the_very_large_interacting_galaxy_ngc6872Sérgio Sacani
This document summarizes observations of stars and gas in the interacting galaxy NGC 6872 using radio telescope data and numerical simulations. It finds:
1) NGC 6872 contains 1.4x1010 solar masses of atomic hydrogen gas distributed in an extended rotating disk.
2) Massive gas concentrations of about 109 solar masses are detected at the tips of both tidal tails and in the northern optical arm near a companion galaxy.
3) Simulations reproducing the galaxy's morphology, inner bar, tidal tail extent and thinness support a gravitational interaction scenario with a small nearby companion galaxy.
Three newly discovered_globular_clusters_in_ngc6822Sérgio Sacani
This document describes the discovery of three new globular clusters in the Local Group dwarf irregular galaxy NGC 6822. The authors present optical photometry of the clusters from archival CFHT/Megacam data. Two clusters are luminous and compact, while the third is a lower luminosity diffuse cluster. The positions of the new clusters are consistent with the linear alignment of previously known clusters in NGC 6822. Studying globular cluster systems in dwarf galaxies provides insights into the formation of larger galaxies through accretion and mergers.
Shaping the glowing_eye_planetary_nebula_ngc6751Sérgio Sacani
This document presents a comprehensive study of the planetary nebula NGC 6751 using spectroscopic observations and imaging. It finds:
1) NGC 6751 has a thick equatorial ring fragmented into knots enclosing a central bubble, surrounded by faint envelope and bipolar lobes with filaments.
2) Kinematic data identify distinct velocities for different components: the outer halo at -15 km/s, inner halo at -31 km/s, and bipolar lobes at ±30 km/s.
3) A 3D morpho-kinematic model is constructed using the SHAPE code that closely matches the observed images and spectra, providing insight into the nebula's complex structure.
This document summarizes observations of IGR J12580+0134, a newly discovered hard X-ray source associated with the Seyfert 2 galaxy NGC 4845, which underwent an unusual X-ray flare. Follow-up observations with XMM-Newton, Swift, MAXI, and INTEGRAL are presented and analyzed. The spectrum is well described by an absorbed power law plus soft excess. The hard X-ray flux increased over weeks and decreased over a year as expected for a tidal disruption event. Fast variations near peak allowed estimating the black hole mass as ∼3×105 M⊙, indicating disruption of ∼10% of a 14-30 Jupiter mass object. Hard X-ray emission is from a corona forming
The document summarizes two Chandra X-ray observations of the Type IIn supernova SN 2010jl taken around two months and one year after explosion. The first observation revealed a high temperature (10 keV) and very high absorption column density (1024 cm-2) from circumstellar matter. The second observation, one year later, showed the absorption column had decreased by a factor of three as expected from shock propagation. Both observations detected an unabsorbed luminosity of 7×1041 erg s-1. The Fe line detected in the first observation was not present in the second.
1) NGC 474 is a lenticular galaxy surrounded by shells of matter whose origin is still debated - they could have formed from merging with a low mass galaxy or gravitational interaction with satellite galaxy NGC 470.
2) Photometric analysis of NGC 474 found its surface brightness profile is typical for a lenticular galaxy even in the center, and the color indices of the shells are consistent with NGC 474.
3) This implies the shells most likely originated from gravitational interaction with NGC 470 rather than from merging, as merging would have disturbed the central surface brightness profile.
Hoag's Object is a peculiar ring galaxy with a central elliptical core. New observations from Hubble Space Telescope and Russian 6-m telescope provide additional data on its structure and kinematics. The data show Hoag's Object has an old stellar core surrounded by a luminous quasi-spiral pattern and massive HI disk. Previous formation scenarios are reviewed in light of the new data. A new scenario is proposed where the elliptical core formed early in the Universe and the HI disk later formed by cold accretion of primordial gas.
Detection of the_central_star_of_the_planetary_nebula_ngc6302Sérgio Sacani
This document reports on the first direct detection of the central star of the planetary nebula NGC 6302 using the Wide Field Camera 3 on the Hubble Space Telescope. Photometry of the central star was obtained in two narrowband filters, F469N and F673N, from which the reddening was estimated to be c=3.1, corresponding to AV=6.6 magnitudes of extinction. Comparison to evolutionary tracks suggests the central star has a temperature of around 200,000 K, luminosity of 2000 L☉, and the nebula is around 2,200 years old. The high extinction from dust in the nebula had previously prevented direct detection of the central star.
Stars and gas_in_the_very_large_interacting_galaxy_ngc6872Sérgio Sacani
This document summarizes observations of stars and gas in the interacting galaxy NGC 6872 using radio telescope data and numerical simulations. It finds:
1) NGC 6872 contains 1.4x1010 solar masses of atomic hydrogen gas distributed in an extended rotating disk.
2) Massive gas concentrations of about 109 solar masses are detected at the tips of both tidal tails and in the northern optical arm near a companion galaxy.
3) Simulations reproducing the galaxy's morphology, inner bar, tidal tail extent and thinness support a gravitational interaction scenario with a small nearby companion galaxy.
Three newly discovered_globular_clusters_in_ngc6822Sérgio Sacani
This document describes the discovery of three new globular clusters in the Local Group dwarf irregular galaxy NGC 6822. The authors present optical photometry of the clusters from archival CFHT/Megacam data. Two clusters are luminous and compact, while the third is a lower luminosity diffuse cluster. The positions of the new clusters are consistent with the linear alignment of previously known clusters in NGC 6822. Studying globular cluster systems in dwarf galaxies provides insights into the formation of larger galaxies through accretion and mergers.
Shaping the glowing_eye_planetary_nebula_ngc6751Sérgio Sacani
This document presents a comprehensive study of the planetary nebula NGC 6751 using spectroscopic observations and imaging. It finds:
1) NGC 6751 has a thick equatorial ring fragmented into knots enclosing a central bubble, surrounded by faint envelope and bipolar lobes with filaments.
2) Kinematic data identify distinct velocities for different components: the outer halo at -15 km/s, inner halo at -31 km/s, and bipolar lobes at ±30 km/s.
3) A 3D morpho-kinematic model is constructed using the SHAPE code that closely matches the observed images and spectra, providing insight into the nebula's complex structure.
This document summarizes observations of IGR J12580+0134, a newly discovered hard X-ray source associated with the Seyfert 2 galaxy NGC 4845, which underwent an unusual X-ray flare. Follow-up observations with XMM-Newton, Swift, MAXI, and INTEGRAL are presented and analyzed. The spectrum is well described by an absorbed power law plus soft excess. The hard X-ray flux increased over weeks and decreased over a year as expected for a tidal disruption event. Fast variations near peak allowed estimating the black hole mass as ∼3×105 M⊙, indicating disruption of ∼10% of a 14-30 Jupiter mass object. Hard X-ray emission is from a corona forming
The document summarizes two Chandra X-ray observations of the Type IIn supernova SN 2010jl taken around two months and one year after explosion. The first observation revealed a high temperature (10 keV) and very high absorption column density (1024 cm-2) from circumstellar matter. The second observation, one year later, showed the absorption column had decreased by a factor of three as expected from shock propagation. Both observations detected an unabsorbed luminosity of 7×1041 erg s-1. The Fe line detected in the first observation was not present in the second.
1) NGC 474 is a lenticular galaxy surrounded by shells of matter whose origin is still debated - they could have formed from merging with a low mass galaxy or gravitational interaction with satellite galaxy NGC 470.
2) Photometric analysis of NGC 474 found its surface brightness profile is typical for a lenticular galaxy even in the center, and the color indices of the shells are consistent with NGC 474.
3) This implies the shells most likely originated from gravitational interaction with NGC 470 rather than from merging, as merging would have disturbed the central surface brightness profile.
Hoag's Object is a peculiar ring galaxy with a central elliptical core. New observations from Hubble Space Telescope and Russian 6-m telescope provide additional data on its structure and kinematics. The data show Hoag's Object has an old stellar core surrounded by a luminous quasi-spiral pattern and massive HI disk. Previous formation scenarios are reviewed in light of the new data. A new scenario is proposed where the elliptical core formed early in the Universe and the HI disk later formed by cold accretion of primordial gas.
This document summarizes a study that used optical, infrared, and submillimeter data to examine star formation in the region surrounding the IC 348 star cluster and the nearby Flying Ghost Nebula. The study identified 13 protostars driving protostellar outflows in the region, including HH 211 which had not previously been detected at visible wavelengths. The region surrounding the Flying Ghost Nebula shows ongoing star formation with outflows similar to other areas of moderate star formation in Perseus. A candidate bent jet was also found, which may have been ejected from a multiple star system near IC 348.
Ngc1912 and ngc 1907_close_encounter_between_open_clustersSérgio Sacani
1) The open clusters NGC 1912 and NGC 1907 have a projected separation of 18.8 pc and similar distances and ages based on previous studies, suggesting they may be a physical pair.
2) New simulations of the clusters' orbits over the past 200 Myr using their spatial velocities show they were born in different regions of the Galaxy and are currently experiencing a close fly-by encounter.
3) Detailed N-body simulations of the clusters' approach support the conclusion that while they have a close projected proximity now, NGC 1912 and NGC 1907 did not originate from the same star-forming complex and are not a true physical pair.
The identification of_93_day_periodic_photometric_variability_for_yso_ylw_16aSérgio Sacani
This study identifies a 93 day periodic photometric variability in the Class I young stellar object (YSO) YLW 16A in the Rho Ophiuchus star forming region. Light curve analysis reveals variations of ~0.5 magnitudes in the Ks band over this period. The authors propose a triple system model consisting of an inner binary with a 93 day period eclipsed by a warped circumbinary disk, with a tertiary companion at ~40 AU responsible for warping the disk. This model is similar to one previously proposed for another YSO, WL 4, and may indicate such triple systems with eclipsing disks are common around young stars. Understanding these systems can provide insights into stellar and planetary formation and evolution.
This document summarizes a study of the galaxy NGC 3801 using panchromatic data from radio, ultraviolet, optical and infrared wavelengths. The study finds that NGC 3801 is a post-merger early-type galaxy that shows evidence of recent star formation in spiral wisps as well as feedback from active galactic nucleus jets. Specifically, the galaxy has a young radio jet that has not yet impacted the outer gaseous regions, but will likely quench star formation within the next 10 million years and further transform the galaxy into a red elliptical. The multi-wavelength data reveal complex gas and dust structures that may be due to a kinematically decoupled core or warped disk.
The broad lined_type_ic_sn_2012_ap_and_the_nature_of_relatvistic_supernovae_l...Sérgio Sacani
Artigo mostra como os astrônomos deduziram que a supernova SN 2012ap, é o elo perdido que faltava para a construção completa da árvore genealógica das supernovas.
The central star_of_the_planetary_nebula_ngc_6537Sérgio Sacani
1) HST images of the planetary nebula NGC 6537 fail to detect its central star, placing an upper limit on its magnitude of fainter than 22.4.
2) This limit is used to derive a lower limit for the star's temperature of at least 500,000 K based on Zanstra temperature analysis.
3) The energy balance temperature method, which does not require direct observation of the star, yields a temperature consistent with 500,000 K, as does the ionization state of the nebula.
Investigating the nuclear_activity_of_ngc1672Sérgio Sacani
1) The document investigates the nuclear activity of the barred spiral galaxy NGC 1672 using X-ray data from Chandra and XMM-Newton, as well as optical data from Hubble and infrared data from Spitzer.
2) It detects 28 X-ray sources within NGC 1672, with nine being ultraluminous X-ray sources located at the ends of the galaxy's bar.
3) For the first time, it shows NGC 1672 possesses a hard nuclear X-ray source surrounded by an X-ray bright circumnuclear star-forming ring, which dominates the central X-ray emission of the galaxy. The data indicates the nuclear source is a low-luminosity active gal
Creation of cosmic structure in the complex galaxy cluster merger abell 2744Sérgio Sacani
Abell 2744 is one of the most actively merging galaxy clusters known, appearing to have "dark", "ghost", "bullet", and "stripped" substructures of around 1014 solar masses each. The cluster shows a complex phenomenology that will challenge simulations to reproduce. The authors present a detailed strong lensing, weak lensing, and X-ray analysis of Abell 2744, identifying 34 strongly lensed images around the massive Southern core and producing the most detailed mass map to date. They find evidence that the Southern core and Northwestern substructure are post-merger systems similar to the Bullet Cluster viewed from an angle, and derive a new constraint on the self-interaction cross section of dark matter particles. They
Rapid disappearance of a warm dusty circumstellar diskCarlos Bella
- The star TYC 8241 2652 1 was observed to have a factor of 30 decrease in mid-infrared dust emission over less than two years, indicating the rapid disappearance of warm, dusty material orbiting the star.
- Observations before 2009 showed significant mid-infrared excess emission, but 2010 observations and later showed the excess had reduced to barely detectable levels.
- No currently available physical model can satisfactorily explain these rapid changes, which suggest a phase of very rapid evolution of dusty planetary collision ejecta that had not been previously predicted or observed.
Hard xray emission_in_the_star_formation_region_on2Sérgio Sacani
This document reports on XMM-Newton observations of the star-forming region ON 2 and the massive star cluster Berkeley 87. Diffuse hard X-ray emission was detected from two regions within ON 2 - the northern region ON 2N, encompassing the H II regions GAL 75.84+0.40 and GAL 75.84+0.36, and the southern region ON 2S adjacent to the ultra-compact H II region Cygnus 2N. The emission from ON 2N has a luminosity of 10^32 erg/s and can be fit by either a thermal plasma model above 30 MK or a power-law model with gamma=-2.6. The emission from ON 2S has a
Analysis of the recent progress in LENR (cold fusion) by using of BSM-SG atomic models
(A talk presented at the 4-th International conference on nanotechnology Nanotek & Expo, 1-3 Dec 2014, San Francisco),
The new approach provides practical considerations for selection of the elements and their isotopes suitable for cold fusion energy and minimization of the radioactive waste.
Graphical 3D Modeling of Molecules and Nanostructures in Sub-nanometer Scale ...Stoyan Sarg Sargoytchev
The Basic Structures of Matter – Supergravitation Unified Theory (BSM-SG) reveals non-spherical shapes of the stable elementary particles, composed of two types of helical structures with opposite twisting. Proton and neutron have one and the same toroidal sub-structure, but the shape of proton is a twisted torus like the figure 8, while the neutron is a double folded. The shape of proton permits modulation of the space fabrics creating a positive E-field. At neutron such modulation is locked in the near field, so it is not detectable, but when in motion it creates a magnetic field. Due to it’s near E-field the neutron is stable over the proton, forming a deuteron. The electron is a different three body system with two intrinsic frequencies. Its structure and dynamic properties provide classical explanations of: Compton frequency, anomalous magnetic moment, spin and relativistic effect of mass increase. The near Coulomb field of the proton defines the trace of orbiting electron. The atomic nuclei are 3D compositions of protons and neutrons, kept by the attractive supergravitational forces, while balancing the repulsive forces between protons. The increase of number of protons reveals the build-up trend of the atomic nuclei showing a perfect match with the pattern of the Periodic Table. The features defining the valences and the angular restrictions of the chemical bonds are apparent. The rotational freedom of neutrons over protons is behind the nuclear magnetic moment. The BSM-SG atomic models are convenient for 3D graphical modeling of complex molecules and nanostructures with sub-nanometer resolution.
Theoretical Feasibility of Cold Fusion According to the BSM-SG Unified TheoryStoyan Sarg Sargoytchev
Report at 31 Annual Meeting of SSE, 2012
Advances in the field of cold fusion or LENR need a deeper understanding of the nuclear reactions and, more particularly, the possibility for modification of the Coulomb barrier. The treatise “Basic Structures of Matter – Supergravitation Unified Theory”, based on an alternative concept of the physical vacuum, suggests non spherical shapes of the protons and neutrons. Held by strong nuclear forces the non-spherical protons and neutrons form atomic nuclei as fractal three-dimensional structures. Such nuclear structures exhibit an excellent match to the pattern of Periodic Table, showing signatures of valences, and angular restrictions of the chemical bonds. The Coulomb barrier in these nuclear structures does not converge to a small size according to the Bohr nuclear model and it could be modified by some technical methods. The analysis of some cold fusion experiments, using BSM-SG model, resulted for practical and suggestions for other nuclear reactions.
Video-record: http://www.youtube.com/watch?v=S3gJp8rLHWg
1. INTEGRAL observations of the SNR IC443 region detected several sources, including the pulsar wind nebula (Src #5) and the enigmatic hard X-ray source Src #11.
2. JEM-X images in the 6-10 and 10-20 keV bands tentatively identified counterparts for Src #5 and Src #11. Measured fluxes from JEM-X were consistent with XMM spectra but did not provide strong constraints.
3. Optical and infrared images showed possible counterparts for Src #11, including point sources and diffuse 2MASS-Ks emission thought to originate from shocked molecular hydrogen, suggesting a correlation between X-ray and infrared emission.
This document summarizes a study that identified 195 compact elliptical galaxies across different environments using data from optical and ultraviolet sky surveys. The researchers constructed the sample by selecting galaxies that were outliers from the universal color-magnitude relation and had small sizes and high stellar velocity dispersions based on spectral modeling. They found that 7 of the galaxies were isolated, not belonging to any known galaxy groups. For these isolated galaxies, the researchers identified possible host galaxies located up to 3.3 Mpc away. The stellar populations of the isolated compact elliptical galaxies were found to be similar to those in galaxy groups and clusters, suggesting a common formation mechanism.
Gravito-inertial Propulsion effect Predicted by the BSM - Supergravitation Un...Stoyan Sarg Sargoytchev
Report at 27 Annual SSE meeting 2008.
The Basic Structures of Matter - Supergravitation Unified Theory (BSM-SG) is based on an alternative concept of the physical vacuum. The suggested model works well in different fields of Physics. More importantly it permit to understand the relation between the Quantum Mechanics, Relativity and Newtonian Physics leading to new understanding of the gravity and inertia. By proper modulation the parameters of the physical vacuum, the gravito-inertial mass of a specifically designed spacecraft would be reduced, so it could be accelerated with less energy. Technically the new space drive mechanism could be realized by electromagnetically activated neutral plasma surrounding the spacecraft. In such approach secondary effects, such as optical glow, hissing noise, light bending and disturbed propagation of EM waves and Earth magnetic field would take place in the surrounding zone. The predicted space drive will work not only in the earth atmosphere but also in a deep space, if the spacecraft is surrounded by EM activated plasma.
Video-record: http://www.youtube.com/watch?v=s5ypGrw5q1w
No signature of_ejecta_interaction_with_a_stellar_companion_in_three_type_ia_...Sérgio Sacani
ARtigo descreve estudos de supernovas feitos com o Kepler e mostram que explosões podem ser geradas por estrelas anãs brancas simples, se chocando com outras ou se fundindo com outras.
The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...Sérgio Sacani
The document summarizes a study of an extreme molecular cloud in the Antennae galaxies that has properties consistent with forming a globular cluster. ALMA observations reveal a cloud with a radius of 24 pc and mass greater than 5 million solar masses. While capable of forming a globular cluster, a lack of associated thermal radio emission indicates star formation has not yet begun to alter the environment, suggesting the cloud is in an early stage of evolution. For the cloud to be confined as observed, an external pressure over 10,000 times greater than typical interstellar pressure is required, supporting the theory that high pressures are needed to form globular clusters in extreme environments like mergers.
This document describes an educational activity to calculate the Earth-Sun distance from images of the transit of Venus. It discusses:
1) The objectives of calculating a physical parameter (Earth-Sun distance) by applying mathematics and image analysis skills.
2) The transit of Venus phenomenon, including its rarity, previous transits observed, and effects seen like the "black drop" and "Venus aureole."
3) The methodology that will be used - measuring the parallax of Venus through simultaneous images from two locations, and using trigonometry to calculate the Earth-Sun distance from the parallax measurements.
This document summarizes a study of physical conditions in Barnard's Loop and the Orion-Eridanus Bubble, and implications for the Warm Ionized Medium component of the interstellar medium. The authors present new spectrophotometric observations of Barnard's Loop and use photoionization models to show that Barnard's Loop is photoionized by four candidate stars, but the models only agree with observations if Barnard's Loop has enhanced heavy element abundances by a factor of 1.4. Barnard's Loop resembles the brightest components of the Orion-Eridanus Bubble and Warm Ionized Medium. The models establish conditions that can explain the range of locations in diagnostic diagrams using a limited range of parameters
This document summarizes a study that used optical, infrared, and submillimeter data to examine star formation in the region surrounding the IC 348 star cluster and the nearby Flying Ghost Nebula. The study identified 13 protostars driving protostellar outflows in the region, including HH 211 which had not previously been detected at visible wavelengths. The region surrounding the Flying Ghost Nebula shows ongoing star formation with outflows similar to other areas of moderate star formation in Perseus. A candidate bent jet was also found, which may have been ejected from a multiple star system near IC 348.
Ngc1912 and ngc 1907_close_encounter_between_open_clustersSérgio Sacani
1) The open clusters NGC 1912 and NGC 1907 have a projected separation of 18.8 pc and similar distances and ages based on previous studies, suggesting they may be a physical pair.
2) New simulations of the clusters' orbits over the past 200 Myr using their spatial velocities show they were born in different regions of the Galaxy and are currently experiencing a close fly-by encounter.
3) Detailed N-body simulations of the clusters' approach support the conclusion that while they have a close projected proximity now, NGC 1912 and NGC 1907 did not originate from the same star-forming complex and are not a true physical pair.
The identification of_93_day_periodic_photometric_variability_for_yso_ylw_16aSérgio Sacani
This study identifies a 93 day periodic photometric variability in the Class I young stellar object (YSO) YLW 16A in the Rho Ophiuchus star forming region. Light curve analysis reveals variations of ~0.5 magnitudes in the Ks band over this period. The authors propose a triple system model consisting of an inner binary with a 93 day period eclipsed by a warped circumbinary disk, with a tertiary companion at ~40 AU responsible for warping the disk. This model is similar to one previously proposed for another YSO, WL 4, and may indicate such triple systems with eclipsing disks are common around young stars. Understanding these systems can provide insights into stellar and planetary formation and evolution.
This document summarizes a study of the galaxy NGC 3801 using panchromatic data from radio, ultraviolet, optical and infrared wavelengths. The study finds that NGC 3801 is a post-merger early-type galaxy that shows evidence of recent star formation in spiral wisps as well as feedback from active galactic nucleus jets. Specifically, the galaxy has a young radio jet that has not yet impacted the outer gaseous regions, but will likely quench star formation within the next 10 million years and further transform the galaxy into a red elliptical. The multi-wavelength data reveal complex gas and dust structures that may be due to a kinematically decoupled core or warped disk.
The broad lined_type_ic_sn_2012_ap_and_the_nature_of_relatvistic_supernovae_l...Sérgio Sacani
Artigo mostra como os astrônomos deduziram que a supernova SN 2012ap, é o elo perdido que faltava para a construção completa da árvore genealógica das supernovas.
The central star_of_the_planetary_nebula_ngc_6537Sérgio Sacani
1) HST images of the planetary nebula NGC 6537 fail to detect its central star, placing an upper limit on its magnitude of fainter than 22.4.
2) This limit is used to derive a lower limit for the star's temperature of at least 500,000 K based on Zanstra temperature analysis.
3) The energy balance temperature method, which does not require direct observation of the star, yields a temperature consistent with 500,000 K, as does the ionization state of the nebula.
Investigating the nuclear_activity_of_ngc1672Sérgio Sacani
1) The document investigates the nuclear activity of the barred spiral galaxy NGC 1672 using X-ray data from Chandra and XMM-Newton, as well as optical data from Hubble and infrared data from Spitzer.
2) It detects 28 X-ray sources within NGC 1672, with nine being ultraluminous X-ray sources located at the ends of the galaxy's bar.
3) For the first time, it shows NGC 1672 possesses a hard nuclear X-ray source surrounded by an X-ray bright circumnuclear star-forming ring, which dominates the central X-ray emission of the galaxy. The data indicates the nuclear source is a low-luminosity active gal
Creation of cosmic structure in the complex galaxy cluster merger abell 2744Sérgio Sacani
Abell 2744 is one of the most actively merging galaxy clusters known, appearing to have "dark", "ghost", "bullet", and "stripped" substructures of around 1014 solar masses each. The cluster shows a complex phenomenology that will challenge simulations to reproduce. The authors present a detailed strong lensing, weak lensing, and X-ray analysis of Abell 2744, identifying 34 strongly lensed images around the massive Southern core and producing the most detailed mass map to date. They find evidence that the Southern core and Northwestern substructure are post-merger systems similar to the Bullet Cluster viewed from an angle, and derive a new constraint on the self-interaction cross section of dark matter particles. They
Rapid disappearance of a warm dusty circumstellar diskCarlos Bella
- The star TYC 8241 2652 1 was observed to have a factor of 30 decrease in mid-infrared dust emission over less than two years, indicating the rapid disappearance of warm, dusty material orbiting the star.
- Observations before 2009 showed significant mid-infrared excess emission, but 2010 observations and later showed the excess had reduced to barely detectable levels.
- No currently available physical model can satisfactorily explain these rapid changes, which suggest a phase of very rapid evolution of dusty planetary collision ejecta that had not been previously predicted or observed.
Hard xray emission_in_the_star_formation_region_on2Sérgio Sacani
This document reports on XMM-Newton observations of the star-forming region ON 2 and the massive star cluster Berkeley 87. Diffuse hard X-ray emission was detected from two regions within ON 2 - the northern region ON 2N, encompassing the H II regions GAL 75.84+0.40 and GAL 75.84+0.36, and the southern region ON 2S adjacent to the ultra-compact H II region Cygnus 2N. The emission from ON 2N has a luminosity of 10^32 erg/s and can be fit by either a thermal plasma model above 30 MK or a power-law model with gamma=-2.6. The emission from ON 2S has a
Analysis of the recent progress in LENR (cold fusion) by using of BSM-SG atomic models
(A talk presented at the 4-th International conference on nanotechnology Nanotek & Expo, 1-3 Dec 2014, San Francisco),
The new approach provides practical considerations for selection of the elements and their isotopes suitable for cold fusion energy and minimization of the radioactive waste.
Graphical 3D Modeling of Molecules and Nanostructures in Sub-nanometer Scale ...Stoyan Sarg Sargoytchev
The Basic Structures of Matter – Supergravitation Unified Theory (BSM-SG) reveals non-spherical shapes of the stable elementary particles, composed of two types of helical structures with opposite twisting. Proton and neutron have one and the same toroidal sub-structure, but the shape of proton is a twisted torus like the figure 8, while the neutron is a double folded. The shape of proton permits modulation of the space fabrics creating a positive E-field. At neutron such modulation is locked in the near field, so it is not detectable, but when in motion it creates a magnetic field. Due to it’s near E-field the neutron is stable over the proton, forming a deuteron. The electron is a different three body system with two intrinsic frequencies. Its structure and dynamic properties provide classical explanations of: Compton frequency, anomalous magnetic moment, spin and relativistic effect of mass increase. The near Coulomb field of the proton defines the trace of orbiting electron. The atomic nuclei are 3D compositions of protons and neutrons, kept by the attractive supergravitational forces, while balancing the repulsive forces between protons. The increase of number of protons reveals the build-up trend of the atomic nuclei showing a perfect match with the pattern of the Periodic Table. The features defining the valences and the angular restrictions of the chemical bonds are apparent. The rotational freedom of neutrons over protons is behind the nuclear magnetic moment. The BSM-SG atomic models are convenient for 3D graphical modeling of complex molecules and nanostructures with sub-nanometer resolution.
Theoretical Feasibility of Cold Fusion According to the BSM-SG Unified TheoryStoyan Sarg Sargoytchev
Report at 31 Annual Meeting of SSE, 2012
Advances in the field of cold fusion or LENR need a deeper understanding of the nuclear reactions and, more particularly, the possibility for modification of the Coulomb barrier. The treatise “Basic Structures of Matter – Supergravitation Unified Theory”, based on an alternative concept of the physical vacuum, suggests non spherical shapes of the protons and neutrons. Held by strong nuclear forces the non-spherical protons and neutrons form atomic nuclei as fractal three-dimensional structures. Such nuclear structures exhibit an excellent match to the pattern of Periodic Table, showing signatures of valences, and angular restrictions of the chemical bonds. The Coulomb barrier in these nuclear structures does not converge to a small size according to the Bohr nuclear model and it could be modified by some technical methods. The analysis of some cold fusion experiments, using BSM-SG model, resulted for practical and suggestions for other nuclear reactions.
Video-record: http://www.youtube.com/watch?v=S3gJp8rLHWg
1. INTEGRAL observations of the SNR IC443 region detected several sources, including the pulsar wind nebula (Src #5) and the enigmatic hard X-ray source Src #11.
2. JEM-X images in the 6-10 and 10-20 keV bands tentatively identified counterparts for Src #5 and Src #11. Measured fluxes from JEM-X were consistent with XMM spectra but did not provide strong constraints.
3. Optical and infrared images showed possible counterparts for Src #11, including point sources and diffuse 2MASS-Ks emission thought to originate from shocked molecular hydrogen, suggesting a correlation between X-ray and infrared emission.
This document summarizes a study that identified 195 compact elliptical galaxies across different environments using data from optical and ultraviolet sky surveys. The researchers constructed the sample by selecting galaxies that were outliers from the universal color-magnitude relation and had small sizes and high stellar velocity dispersions based on spectral modeling. They found that 7 of the galaxies were isolated, not belonging to any known galaxy groups. For these isolated galaxies, the researchers identified possible host galaxies located up to 3.3 Mpc away. The stellar populations of the isolated compact elliptical galaxies were found to be similar to those in galaxy groups and clusters, suggesting a common formation mechanism.
Gravito-inertial Propulsion effect Predicted by the BSM - Supergravitation Un...Stoyan Sarg Sargoytchev
Report at 27 Annual SSE meeting 2008.
The Basic Structures of Matter - Supergravitation Unified Theory (BSM-SG) is based on an alternative concept of the physical vacuum. The suggested model works well in different fields of Physics. More importantly it permit to understand the relation between the Quantum Mechanics, Relativity and Newtonian Physics leading to new understanding of the gravity and inertia. By proper modulation the parameters of the physical vacuum, the gravito-inertial mass of a specifically designed spacecraft would be reduced, so it could be accelerated with less energy. Technically the new space drive mechanism could be realized by electromagnetically activated neutral plasma surrounding the spacecraft. In such approach secondary effects, such as optical glow, hissing noise, light bending and disturbed propagation of EM waves and Earth magnetic field would take place in the surrounding zone. The predicted space drive will work not only in the earth atmosphere but also in a deep space, if the spacecraft is surrounded by EM activated plasma.
Video-record: http://www.youtube.com/watch?v=s5ypGrw5q1w
No signature of_ejecta_interaction_with_a_stellar_companion_in_three_type_ia_...Sérgio Sacani
ARtigo descreve estudos de supernovas feitos com o Kepler e mostram que explosões podem ser geradas por estrelas anãs brancas simples, se chocando com outras ou se fundindo com outras.
The physical conditions_in_a_pre_super_star_cluster_molecular_cloud_in_the_an...Sérgio Sacani
The document summarizes a study of an extreme molecular cloud in the Antennae galaxies that has properties consistent with forming a globular cluster. ALMA observations reveal a cloud with a radius of 24 pc and mass greater than 5 million solar masses. While capable of forming a globular cluster, a lack of associated thermal radio emission indicates star formation has not yet begun to alter the environment, suggesting the cloud is in an early stage of evolution. For the cloud to be confined as observed, an external pressure over 10,000 times greater than typical interstellar pressure is required, supporting the theory that high pressures are needed to form globular clusters in extreme environments like mergers.
This document describes an educational activity to calculate the Earth-Sun distance from images of the transit of Venus. It discusses:
1) The objectives of calculating a physical parameter (Earth-Sun distance) by applying mathematics and image analysis skills.
2) The transit of Venus phenomenon, including its rarity, previous transits observed, and effects seen like the "black drop" and "Venus aureole."
3) The methodology that will be used - measuring the parallax of Venus through simultaneous images from two locations, and using trigonometry to calculate the Earth-Sun distance from the parallax measurements.
This document summarizes a study of physical conditions in Barnard's Loop and the Orion-Eridanus Bubble, and implications for the Warm Ionized Medium component of the interstellar medium. The authors present new spectrophotometric observations of Barnard's Loop and use photoionization models to show that Barnard's Loop is photoionized by four candidate stars, but the models only agree with observations if Barnard's Loop has enhanced heavy element abundances by a factor of 1.4. Barnard's Loop resembles the brightest components of the Orion-Eridanus Bubble and Warm Ionized Medium. The models establish conditions that can explain the range of locations in diagnostic diagrams using a limited range of parameters
This document appears to be a citation for a 1995 publication in the journal Astronomy & Astrophysics with the volume number 295 and page number 509, but it provides no other contextual information about the publication itself. The citation is repeated multiple times without any accompanying text.
This document summarizes a study of the young star cluster IC 5146. Optical and near-infrared photometry were obtained for over 700 stars in the region, including around the illuminating stars BD +46°3474 and the embedded variable star BD +46°3471. Around 100 emission-line stars brighter than R=20.5 were found, most in IC 5146. Spectroscopy of 38 stars found an average extinction of AV=3.0 mag. The age distribution of the emission-line stars was estimated from theoretical isochrones to have a median age of around 1 Myr.
An atlas of_predicted_exotic_gravitational_lensesSérgio Sacani
This document discusses an atlas of predicted exotic gravitational lenses. It begins by noting that upcoming wide-field surveys will discover thousands of new strong gravitational lenses, some of which may have unusual image configurations. It then describes using a ray-tracing code to model exotic lenses produced by multi-component galaxy potentials, including lenses with misaligned disks and bulges that produce "broken" Einstein rings, and binary or merging galaxies that produce a Y-shaped image configuration. The document estimates the abundance of these exotic galaxy-scale lenses to be approximately one per all-sky survey. It also discusses how cluster lenses can produce a wide range of caustic structures, and interprets the central ring and counter-image in Abell 1703 as
This document summarizes observations of the giant exoplanet τ Boötis b using high-resolution spectroscopy to detect carbon monoxide absorption in the planet's atmosphere. Key findings include:
1) The observations trace the planet's radial velocity over its orbit, determining an orbital inclination of 44.5±1.5 degrees and true planet mass of 5.95±0.28 Jupiter masses.
2) Carbon monoxide absorption indicates the planet's atmosphere has a temperature decreasing with altitude rather than a thermal inversion, contrasting with other highly irradiated planets.
3) This supports models where strong UV radiation from the active host star destroys compounds causing thermal inversions in other planets' atmospheres.
1) NGC 474 is a lenticular galaxy surrounded by shells of matter whose origin is still debated.
2) Through surface photometry, the authors found that NGC 474's surface brightness profile is typical for a lenticular galaxy even in its central parts, and the color indices of the shells are consistent with NGC 474.
3) This implies that the shells likely originated from gravitational interaction with the nearby satellite galaxy NGC 470 rather than from the merging of two galaxies, as mergers would have disturbed NGC 474's central regions.
This document summarizes a study of the Ara OB1a stellar association based on new optical photometry. The photometry was used to estimate the fundamental parameters of two prominent clusters in the association, NGC 6167 and NGC 6193, as well as the IRAS 16375-4854 source. NGC 6167 was found to be an intermediate-age cluster of 20-30 Myr, while NGC 6193 is very young at 1-5 Myr with evidence of ongoing star formation. The IRAS source is the youngest, containing several young stellar objects. The differences in ages support a picture of sequential star formation triggered over several tens of million years in the Ara OB1a region.
This document summarizes a study of the Ara OB1a stellar association based on new optical photometry. The key findings are:
1) New UBVIC and Hα photometry is presented to provide more robust estimates of the fundamental parameters (age and distance) of the two prominent clusters NGC 6167 and NGC 6193.
2) NGC 6167 is found to be an intermediate-age cluster (20-30 Myr), NGC 6193 a very young one (1-5 Myr) containing pre-main sequence stars and Hα emitters.
3) The youngest object is the IRAS 16375-4854 source, containing several young stellar objects. This supports sequential star formation
This document summarizes observations from integral field spectroscopy of the low-luminosity Seyfert galaxy NGC 5033 using the INTEGRAL system on the William Herschel Telescope. The Hβ emission line map shows a spiral or ring-like pattern of HII regions, while the [OIII] map shows a markedly asymmetric morphology, indicating ionized gas illuminated by the active galactic nucleus. Kinematic analysis reveals important deviations between the [OIII] emitters and stellar velocity field, related to the asymmetric ionization structure. The Seyfert 1 nucleus is identified by its broad Hβ emission and located in an obscured region with the bluest spectral energy distribution.
Off nuclear star_formation_and_obscured_activity_in_the_luminous_infrared_gal...Sérgio Sacani
The document summarizes observations of the luminous infrared galaxy NGC 2623 from multiple telescopes. Hubble Space Telescope images reveal over 100 bright star clusters in a 3.2 kpc extension south of the galaxy's nucleus, making it one of the richest concentrations of clusters observed. The clusters have ages between 1-100 Myr based on their optical colors. Archival GALEX data show the extension is very bright in far-ultraviolet but less significant at longer wavelengths. Spitzer data detect [Ne V] emission, confirming the presence of an active galactic nucleus. The off-nuclear star formation corresponds to a rate of 0.1-0.2 solar masses per year, while the bulk of the infrared
The document presents observations of the starburst galaxy NGC 253 using near-infrared imaging and spectroscopy as well as mid-infrared spectroscopy. The observations are used to derive physical properties of the starburst such as the star formation rate, stellar population, and evolutionary stage. Evolutionary synthesis modeling is applied to interpret the observations and show that the starburst in NGC 253 is in a late phase, has been ongoing for 20-30 million years, and is consistent with a modified Salpeter initial mass function.
Star formation history_in_the_smc_the_case_of_ngc602Sérgio Sacani
This document summarizes a study of the star formation history in the NGC 602 region of the Small Magellanic Cloud based on Hubble Space Telescope observations. Deep photometry reveals numerous pre-main sequence stars as well as young stars on the main sequence, allowing the study of star formation into recent times. New pre-main sequence stellar evolutionary tracks are presented. A stellar population synthesis code is used to derive the best estimate of the star formation history by comparing observed and synthetic color-magnitude diagrams. The star formation rate in the region has increased over the past tens of Myr, reaching 0.3-0.7×10−3 M☉ yr−1 in the last 2.5 Myr, comparable to
Extended x ray emission in the h i cavity of ngc 4151- galaxy-scale active ga...Sérgio Sacani
The document summarizes the discovery of diffuse soft X-ray emission extending about 2 kpc from the active nucleus of NGC 4151, filling the cavity of H i material. The X-ray emission has a luminosity of about 1039 erg s-1 and can be fit with either a thermal plasma model with a temperature of around 0.25 keV, or a photoionized model. This interaction between the AGN and interstellar medium implies the last episode of high nuclear activity occurred relatively recently, around 104 years ago.
This document summarizes a study on the formation of polar ring galaxies through two proposed scenarios: the merging scenario and the accretion scenario. The merging scenario involves a head-on collision between two galaxies, where one becomes the host galaxy and the other's gas forms the polar ring. The accretion scenario involves tidal interactions that allow gas from one galaxy to be accreted by another galaxy to form a polar ring. Through simulations, the study finds that both scenarios can produce stable polar rings, but that the accretion scenario better matches observed properties of polar ring galaxies, such as the frequency and morphology of the rings. The study concludes the accretion scenario is both more likely and more supported by observations to explain how most polar ring galaxies form.
This document reports the discovery of the central star of the planetary nebula IC 4663, which exhibits spectral properties that mimic a nitrogen-rich Wolf-Rayet star of spectral type [WN3]. This makes it the first unambiguous case of a planetary nebula central star taking on the properties of a Wolf-Rayet star. The central star is dominated by broad helium and nitrogen emission lines. The surrounding nebula is definitively a planetary nebula based on its morphology and chemical abundances. The discovery provides evidence for an alternative evolutionary pathway for some hydrogen-deficient, helium-rich post-asymptotic giant branch stars.
The exceptional soft_x_ray_halo_of_the_galaxy_merger_ngc6240Sérgio Sacani
The document summarizes a recent 150-ks Chandra observation of the galaxy merger NGC 6240. Extended soft X-ray emission is detected over a 110x80 kpc region around NGC 6240. Spectral analysis finds the emission comes from hot gas with a temperature of around 7.5 million K and a total mass of about 10^10 solar masses. The gas properties suggest widespread star formation over the past 200 Myr rather than a recent nuclear starburst. The fate of the diffuse hot gas after the galaxy merger is uncertain but it may be retained and evolve into the halo of an elliptical galaxy.
The document summarizes new HST NICMOS observations of the galaxy NGC 4945, which hosts an active galactic nucleus that is highly obscured at optical and mid-infrared wavelengths. A 100pc starburst ring is detected in Paα emission, while H2 traces the walls of a superbubble opened by supernova-driven winds. No direct evidence of the active nucleus is found in the near-infrared observations. However, it is not possible to conclusively determine if the bolometric luminosity is powered by the AGN or starburst based on the available data. The observations demonstrate that powerful AGNs can still be hidden even at mid-infrared wavelengths, and multi-wavelength data including hard X-rays is
Models of the_intergalactic_gas_in_stephan_quintetSérgio Sacani
This document summarizes a numerical simulation study of the intergalactic gas in Stephan's Quintet galaxy group. The simulation uses smoothed particle hydrodynamics to model the formation of hot X-ray gas, large-scale shocks, and emission line gas seen in observations, as NGC 7318b collides with the group. The simulation reproduces the general morphology of the group, but requires adjustments to better match velocities and temperatures seen in radio, X-ray, and infrared observations. Future work will fine-tune the model parameters and cooling processes to improve agreement with multi-wavelength data.
This document summarizes the discovery and analysis of a Type Ia supernova (SN Ia) at a redshift of 1.71, the most distant spectroscopically confirmed SN Ia at the time. The Hubble Space Telescope was used to obtain spectroscopy and photometry of the supernova. Analysis of the spectroscopy confirms it as a SN Ia with 92% confidence. The photometry is used to determine the supernova's distance, which agrees with the predictions of the ΛCDM cosmological model. This distant supernova helps improve constraints on the nature and behavior of dark energy in the early universe.
This document summarizes a study that uses U-band photometry to determine photometric distances to young stars in the inner Galactic disk. The study focuses on the line of sight towards the Galactic longitude of 314 degrees. Photometric data is collected and calibrated using two open clusters in the field. Three groups of stars are detected at distances of 1.5, 2.5, and 5.1 kpc, which are consistent with the Carina-Sagittarius and Scutum-Crux spiral arms. The use of U-band photometry is shown to be an effective method for characterizing young star populations and making predictions about spiral structure in the Milky Way.
The intermediate age_open_cluster_ngc2158Sérgio Sacani
This document presents a study of the intermediate-age open cluster NGC 2158 based on UBVRI CCD photometry. The key findings are:
1) The color-magnitude diagrams show a prominent red giant clump at V ≈ 15.0, (B-V) ≈ 1.5 and a turn-off point at V ≈ 16.0, (B-V) ≈ 1.0.
2) Analysis of the (B-I) vs (B-V) diagram yields a mean reddening of EB-V = 0.55 ± 0.10 for the cluster.
3) The elongated shape of the red giant clump in the CMD is
This document summarizes a study of the outer rings of supernova SN 1987A using spectroscopy and archival Hubble Space Telescope images spanning 11 years. The study finds:
1) Light curves of emission lines from the outer rings show a declining behavior, consistent with initial supernova flash powering.
2) Electron densities in the outer rings are <3,000 cm-3 and have not changed in 15 years. Temperature remains at ~12,000 K.
3) Densities may be highest (~5,000 cm-3) in the southern outer ring, which shows slightly faster decline in H-alpha emission.
4) Interaction between supernova ejecta and outer rings could begin within ~
We discovered two transient events in the Kepler eld with light curves that strongly suggest they
are type II-P supernovae. Using the fast cadence of the Kepler observations we precisely estimate
the rise time to maximum for KSN2011a and KSN2011d as 10.50:4 and 13.30:4 rest-frame days
respectively. Based on ts to idealized analytic models, we nd the progenitor radius of KSN2011a
(28020 R) to be signicantly smaller than that for KSN2011d (49020 R) but both have similar
explosion energies of 2.00:3 1051 erg.
The rising light curve of KSN2011d is an excellent match to that predicted by simple models of
exploding red supergiants (RSG). However, the early rise of KSN2011a is faster than the models
predict possibly due to the supernova shockwave moving into pre-existing wind or mass-loss from the
RSG. A mass loss rate of 10 4 M yr 1 from the RSG can explain the fast rise without impacting
the optical
ux at maximum light or the shape of the post-maximum light curve.
No shock breakout emission is seen in KSN2011a, but this is likely due to the circumstellar inter-
action suspected in the fast rising light curve. The early light curve of KSN2011d does show excess
emission consistent with model predictions of a shock breakout. This is the rst optical detection of
a shock breakout from a type II-P supernova.
The origin and_motion_of_pulsar_in_simeis_147Sérgio Sacani
This document summarizes a study measuring the parallax and proper motion of the pulsar PSR J0538+2817 located within the supernova remnant S147 using VLBA radio astrometry over multiple epochs. They determine a distance of 1.47+0.42 kpc and a high transverse velocity of 400+114 km/s for the pulsar. A small extended X-ray nebula is also detected around the pulsar. The proper motion direction suggests the pulsar was born near the geometric center of the remnant and has since moved away, with an inferred kinematic age of around 40,000 years.
Modulations in the_radio_light_curve_of_the_typeiib_supernova_2001igSérgio Sacani
This document summarizes radio observations of the Type IIb supernova SN 2001ig made with the Australia Telescope Compact Array and Very Large Array over 700 days. The observations found periodic deviations from the standard model of radio light curves that are consistent with recurring density modulations in the circumstellar medium with a period of around 150 days. This provides evidence that the progenitor was a Wolf-Rayet star in a binary system with an eccentric 100 day orbit, causing regular build-up of circumstellar material. Such binary systems are thought to produce Type Ib/c supernovae through envelope stripping, linking these events to Type IIb supernovae.
Similar to The stellar content_of_the_ring_in_ngc660 (20)
Compositions of iron-meteorite parent bodies constrainthe structure of the pr...Sérgio Sacani
Magmatic iron-meteorite parent bodies are the earliest planetesimals in the Solar System,and they preserve information about conditions and planet-forming processes in thesolar nebula. In this study, we include comprehensive elemental compositions andfractional-crystallization modeling for iron meteorites from the cores of five differenti-ated asteroids from the inner Solar System. Together with previous results of metalliccores from the outer Solar System, we conclude that asteroidal cores from the outerSolar System have smaller sizes, elevated siderophile-element abundances, and simplercrystallization processes than those from the inner Solar System. These differences arerelated to the formation locations of the parent asteroids because the solar protoplane-tary disk varied in redox conditions, elemental distributions, and dynamics at differentheliocentric distances. Using highly siderophile-element data from iron meteorites, wereconstruct the distribution of calcium-aluminum-rich inclusions (CAIs) across theprotoplanetary disk within the first million years of Solar-System history. CAIs, the firstsolids to condense in the Solar System, formed close to the Sun. They were, however,concentrated within the outer disk and depleted within the inner disk. Future modelsof the structure and evolution of the protoplanetary disk should account for this dis-tribution pattern of CAIs.
Signatures of wave erosion in Titan’s coastsSérgio Sacani
The shorelines of Titan’s hydrocarbon seas trace flooded erosional landforms such as river valleys; however, it isunclear whether coastal erosion has subsequently altered these shorelines. Spacecraft observations and theo-retical models suggest that wind may cause waves to form on Titan’s seas, potentially driving coastal erosion,but the observational evidence of waves is indirect, and the processes affecting shoreline evolution on Titanremain unknown. No widely accepted framework exists for using shoreline morphology to quantitatively dis-cern coastal erosion mechanisms, even on Earth, where the dominant mechanisms are known. We combinelandscape evolution models with measurements of shoreline shape on Earth to characterize how differentcoastal erosion mechanisms affect shoreline morphology. Applying this framework to Titan, we find that theshorelines of Titan’s seas are most consistent with flooded landscapes that subsequently have been eroded bywaves, rather than a uniform erosional process or no coastal erosion, particularly if wave growth saturates atfetch lengths of tens of kilometers.
SDSS1335+0728: The awakening of a ∼ 106M⊙ black hole⋆Sérgio Sacani
Context. The early-type galaxy SDSS J133519.91+072807.4 (hereafter SDSS1335+0728), which had exhibited no prior optical variations during the preceding two decades, began showing significant nuclear variability in the Zwicky Transient Facility (ZTF) alert stream from December 2019 (as ZTF19acnskyy). This variability behaviour, coupled with the host-galaxy properties, suggests that SDSS1335+0728 hosts a ∼ 106M⊙ black hole (BH) that is currently in the process of ‘turning on’. Aims. We present a multi-wavelength photometric analysis and spectroscopic follow-up performed with the aim of better understanding the origin of the nuclear variations detected in SDSS1335+0728. Methods. We used archival photometry (from WISE, 2MASS, SDSS, GALEX, eROSITA) and spectroscopic data (from SDSS and LAMOST) to study the state of SDSS1335+0728 prior to December 2019, and new observations from Swift, SOAR/Goodman, VLT/X-shooter, and Keck/LRIS taken after its turn-on to characterise its current state. We analysed the variability of SDSS1335+0728 in the X-ray/UV/optical/mid-infrared range, modelled its spectral energy distribution prior to and after December 2019, and studied the evolution of its UV/optical spectra. Results. From our multi-wavelength photometric analysis, we find that: (a) since 2021, the UV flux (from Swift/UVOT observations) is four times brighter than the flux reported by GALEX in 2004; (b) since June 2022, the mid-infrared flux has risen more than two times, and the W1−W2 WISE colour has become redder; and (c) since February 2024, the source has begun showing X-ray emission. From our spectroscopic follow-up, we see that (i) the narrow emission line ratios are now consistent with a more energetic ionising continuum; (ii) broad emission lines are not detected; and (iii) the [OIII] line increased its flux ∼ 3.6 years after the first ZTF alert, which implies a relatively compact narrow-line-emitting region. Conclusions. We conclude that the variations observed in SDSS1335+0728 could be either explained by a ∼ 106M⊙ AGN that is just turning on or by an exotic tidal disruption event (TDE). If the former is true, SDSS1335+0728 is one of the strongest cases of an AGNobserved in the process of activating. If the latter were found to be the case, it would correspond to the longest and faintest TDE ever observed (or another class of still unknown nuclear transient). Future observations of SDSS1335+0728 are crucial to further understand its behaviour. Key words. galaxies: active– accretion, accretion discs– galaxies: individual: SDSS J133519.91+072807.4
Discovery of An Apparent Red, High-Velocity Type Ia Supernova at 𝐳 = 2.9 wi...Sérgio Sacani
We present the JWST discovery of SN 2023adsy, a transient object located in a host galaxy JADES-GS
+
53.13485
−
27.82088
with a host spectroscopic redshift of
2.903
±
0.007
. The transient was identified in deep James Webb Space Telescope (JWST)/NIRCam imaging from the JWST Advanced Deep Extragalactic Survey (JADES) program. Photometric and spectroscopic followup with NIRCam and NIRSpec, respectively, confirm the redshift and yield UV-NIR light-curve, NIR color, and spectroscopic information all consistent with a Type Ia classification. Despite its classification as a likely SN Ia, SN 2023adsy is both fairly red (
�
(
�
−
�
)
∼
0.9
) despite a host galaxy with low-extinction and has a high Ca II velocity (
19
,
000
±
2
,
000
km/s) compared to the general population of SNe Ia. While these characteristics are consistent with some Ca-rich SNe Ia, particularly SN 2016hnk, SN 2023adsy is intrinsically brighter than the low-
�
Ca-rich population. Although such an object is too red for any low-
�
cosmological sample, we apply a fiducial standardization approach to SN 2023adsy and find that the SN 2023adsy luminosity distance measurement is in excellent agreement (
≲
1
�
) with
Λ
CDM. Therefore unlike low-
�
Ca-rich SNe Ia, SN 2023adsy is standardizable and gives no indication that SN Ia standardized luminosities change significantly with redshift. A larger sample of distant SNe Ia is required to determine if SN Ia population characteristics at high-
�
truly diverge from their low-
�
counterparts, and to confirm that standardized luminosities nevertheless remain constant with redshift.
Evidence of Jet Activity from the Secondary Black Hole in the OJ 287 Binary S...Sérgio Sacani
Wereport the study of a huge optical intraday flare on 2021 November 12 at 2 a.m. UT in the blazar OJ287. In the binary black hole model, it is associated with an impact of the secondary black hole on the accretion disk of the primary. Our multifrequency observing campaign was set up to search for such a signature of the impact based on a prediction made 8 yr earlier. The first I-band results of the flare have already been reported by Kishore et al. (2024). Here we combine these data with our monitoring in the R-band. There is a big change in the R–I spectral index by 1.0 ±0.1 between the normal background and the flare, suggesting a new component of radiation. The polarization variation during the rise of the flare suggests the same. The limits on the source size place it most reasonably in the jet of the secondary BH. We then ask why we have not seen this phenomenon before. We show that OJ287 was never before observed with sufficient sensitivity on the night when the flare should have happened according to the binary model. We also study the probability that this flare is just an oversized example of intraday variability using the Krakow data set of intense monitoring between 2015 and 2023. We find that the occurrence of a flare of this size and rapidity is unlikely. In machine-readable Tables 1 and 2, we give the full orbit-linked historical light curve of OJ287 as well as the dense monitoring sample of Krakow.
Candidate young stellar objects in the S-cluster: Kinematic analysis of a sub...Sérgio Sacani
Context. The observation of several L-band emission sources in the S cluster has led to a rich discussion of their nature. However, a definitive answer to the classification of the dusty objects requires an explanation for the detection of compact Doppler-shifted Brγ emission. The ionized hydrogen in combination with the observation of mid-infrared L-band continuum emission suggests that most of these sources are embedded in a dusty envelope. These embedded sources are part of the S-cluster, and their relationship to the S-stars is still under debate. To date, the question of the origin of these two populations has been vague, although all explanations favor migration processes for the individual cluster members. Aims. This work revisits the S-cluster and its dusty members orbiting the supermassive black hole SgrA* on bound Keplerian orbits from a kinematic perspective. The aim is to explore the Keplerian parameters for patterns that might imply a nonrandom distribution of the sample. Additionally, various analytical aspects are considered to address the nature of the dusty sources. Methods. Based on the photometric analysis, we estimated the individual H−K and K−L colors for the source sample and compared the results to known cluster members. The classification revealed a noticeable contrast between the S-stars and the dusty sources. To fit the flux-density distribution, we utilized the radiative transfer code HYPERION and implemented a young stellar object Class I model. We obtained the position angle from the Keplerian fit results; additionally, we analyzed the distribution of the inclinations and the longitudes of the ascending node. Results. The colors of the dusty sources suggest a stellar nature consistent with the spectral energy distribution in the near and midinfrared domains. Furthermore, the evaporation timescales of dusty and gaseous clumps in the vicinity of SgrA* are much shorter ( 2yr) than the epochs covered by the observations (≈15yr). In addition to the strong evidence for the stellar classification of the D-sources, we also find a clear disk-like pattern following the arrangements of S-stars proposed in the literature. Furthermore, we find a global intrinsic inclination for all dusty sources of 60 ± 20◦, implying a common formation process. Conclusions. The pattern of the dusty sources manifested in the distribution of the position angles, inclinations, and longitudes of the ascending node strongly suggests two different scenarios: the main-sequence stars and the dusty stellar S-cluster sources share a common formation history or migrated with a similar formation channel in the vicinity of SgrA*. Alternatively, the gravitational influence of SgrA* in combination with a massive perturber, such as a putative intermediate mass black hole in the IRS 13 cluster, forces the dusty objects and S-stars to follow a particular orbital arrangement. Key words. stars: black holes– stars: formation– Galaxy: center– galaxies: star formation
JAMES WEBB STUDY THE MASSIVE BLACK HOLE SEEDSSérgio Sacani
The pathway(s) to seeding the massive black holes (MBHs) that exist at the heart of galaxies in the present and distant Universe remains an unsolved problem. Here we categorise, describe and quantitatively discuss the formation pathways of both light and heavy seeds. We emphasise that the most recent computational models suggest that rather than a bimodal-like mass spectrum between light and heavy seeds with light at one end and heavy at the other that instead a continuum exists. Light seeds being more ubiquitous and the heavier seeds becoming less and less abundant due the rarer environmental conditions required for their formation. We therefore examine the different mechanisms that give rise to different seed mass spectrums. We show how and why the mechanisms that produce the heaviest seeds are also among the rarest events in the Universe and are hence extremely unlikely to be the seeds for the vast majority of the MBH population. We quantify, within the limits of the current large uncertainties in the seeding processes, the expected number densities of the seed mass spectrum. We argue that light seeds must be at least 103 to 105 times more numerous than heavy seeds to explain the MBH population as a whole. Based on our current understanding of the seed population this makes heavy seeds (Mseed > 103 M⊙) a significantly more likely pathway given that heavy seeds have an abundance pattern than is close to and likely in excess of 10−4 compared to light seeds. Finally, we examine the current state-of-the-art in numerical calculations and recent observations and plot a path forward for near-future advances in both domains.
Anti-Universe And Emergent Gravity and the Dark UniverseSérgio Sacani
Recent theoretical progress indicates that spacetime and gravity emerge together from the entanglement structure of an underlying microscopic theory. These ideas are best understood in Anti-de Sitter space, where they rely on the area law for entanglement entropy. The extension to de Sitter space requires taking into account the entropy and temperature associated with the cosmological horizon. Using insights from string theory, black hole physics and quantum information theory we argue that the positive dark energy leads to a thermal volume law contribution to the entropy that overtakes the area law precisely at the cosmological horizon. Due to the competition between area and volume law entanglement the microscopic de Sitter states do not thermalise at sub-Hubble scales: they exhibit memory effects in the form of an entropy displacement caused by matter. The emergent laws of gravity contain an additional ‘dark’ gravitational force describing the ‘elastic’ response due to the entropy displacement. We derive an estimate of the strength of this extra force in terms of the baryonic mass, Newton’s constant and the Hubble acceleration scale a0 = cH0, and provide evidence for the fact that this additional ‘dark gravity force’ explains the observed phenomena in galaxies and clusters currently attributed to dark matter.
The binding of cosmological structures by massless topological defectsSérgio Sacani
Assuming spherical symmetry and weak field, it is shown that if one solves the Poisson equation or the Einstein field
equations sourced by a topological defect, i.e. a singularity of a very specific form, the result is a localized gravitational
field capable of driving flat rotation (i.e. Keplerian circular orbits at a constant speed for all radii) of test masses on a thin
spherical shell without any underlying mass. Moreover, a large-scale structure which exploits this solution by assembling
concentrically a number of such topological defects can establish a flat stellar or galactic rotation curve, and can also deflect
light in the same manner as an equipotential (isothermal) sphere. Thus, the need for dark matter or modified gravity theory is
mitigated, at least in part.
EWOCS-I: The catalog of X-ray sources in Westerlund 1 from the Extended Weste...Sérgio Sacani
Context. With a mass exceeding several 104 M⊙ and a rich and dense population of massive stars, supermassive young star clusters
represent the most massive star-forming environment that is dominated by the feedback from massive stars and gravitational interactions
among stars.
Aims. In this paper we present the Extended Westerlund 1 and 2 Open Clusters Survey (EWOCS) project, which aims to investigate
the influence of the starburst environment on the formation of stars and planets, and on the evolution of both low and high mass stars.
The primary targets of this project are Westerlund 1 and 2, the closest supermassive star clusters to the Sun.
Methods. The project is based primarily on recent observations conducted with the Chandra and JWST observatories. Specifically,
the Chandra survey of Westerlund 1 consists of 36 new ACIS-I observations, nearly co-pointed, for a total exposure time of 1 Msec.
Additionally, we included 8 archival Chandra/ACIS-S observations. This paper presents the resulting catalog of X-ray sources within
and around Westerlund 1. Sources were detected by combining various existing methods, and photon extraction and source validation
were carried out using the ACIS-Extract software.
Results. The EWOCS X-ray catalog comprises 5963 validated sources out of the 9420 initially provided to ACIS-Extract, reaching a
photon flux threshold of approximately 2 × 10−8 photons cm−2
s
−1
. The X-ray sources exhibit a highly concentrated spatial distribution,
with 1075 sources located within the central 1 arcmin. We have successfully detected X-ray emissions from 126 out of the 166 known
massive stars of the cluster, and we have collected over 71 000 photons from the magnetar CXO J164710.20-455217.
The debris of the ‘last major merger’ is dynamically youngSérgio Sacani
The Milky Way’s (MW) inner stellar halo contains an [Fe/H]-rich component with highly eccentric orbits, often referred to as the
‘last major merger.’ Hypotheses for the origin of this component include Gaia-Sausage/Enceladus (GSE), where the progenitor
collided with the MW proto-disc 8–11 Gyr ago, and the Virgo Radial Merger (VRM), where the progenitor collided with the
MW disc within the last 3 Gyr. These two scenarios make different predictions about observable structure in local phase space,
because the morphology of debris depends on how long it has had to phase mix. The recently identified phase-space folds in Gaia
DR3 have positive caustic velocities, making them fundamentally different than the phase-mixed chevrons found in simulations
at late times. Roughly 20 per cent of the stars in the prograde local stellar halo are associated with the observed caustics. Based
on a simple phase-mixing model, the observed number of caustics are consistent with a merger that occurred 1–2 Gyr ago.
We also compare the observed phase-space distribution to FIRE-2 Latte simulations of GSE-like mergers, using a quantitative
measurement of phase mixing (2D causticality). The observed local phase-space distribution best matches the simulated data
1–2 Gyr after collision, and certainly not later than 3 Gyr. This is further evidence that the progenitor of the ‘last major merger’
did not collide with the MW proto-disc at early times, as is thought for the GSE, but instead collided with the MW disc within
the last few Gyr, consistent with the body of work surrounding the VRM.
Observation of Io’s Resurfacing via Plume Deposition Using Ground-based Adapt...Sérgio Sacani
Since volcanic activity was first discovered on Io from Voyager images in 1979, changes
on Io’s surface have been monitored from both spacecraft and ground-based telescopes.
Here, we present the highest spatial resolution images of Io ever obtained from a groundbased telescope. These images, acquired by the SHARK-VIS instrument on the Large
Binocular Telescope, show evidence of a major resurfacing event on Io’s trailing hemisphere. When compared to the most recent spacecraft images, the SHARK-VIS images
show that a plume deposit from a powerful eruption at Pillan Patera has covered part
of the long-lived Pele plume deposit. Although this type of resurfacing event may be common on Io, few have been detected due to the rarity of spacecraft visits and the previously low spatial resolution available from Earth-based telescopes. The SHARK-VIS instrument ushers in a new era of high resolution imaging of Io’s surface using adaptive
optics at visible wavelengths.
Earliest Galaxies in the JADES Origins Field: Luminosity Function and Cosmic ...Sérgio Sacani
We characterize the earliest galaxy population in the JADES Origins Field (JOF), the deepest
imaging field observed with JWST. We make use of the ancillary Hubble optical images (5 filters
spanning 0.4−0.9µm) and novel JWST images with 14 filters spanning 0.8−5µm, including 7 mediumband filters, and reaching total exposure times of up to 46 hours per filter. We combine all our data
at > 2.3µm to construct an ultradeep image, reaching as deep as ≈ 31.4 AB mag in the stack and
30.3-31.0 AB mag (5σ, r = 0.1” circular aperture) in individual filters. We measure photometric
redshifts and use robust selection criteria to identify a sample of eight galaxy candidates at redshifts
z = 11.5 − 15. These objects show compact half-light radii of R1/2 ∼ 50 − 200pc, stellar masses of
M⋆ ∼ 107−108M⊙, and star-formation rates of SFR ∼ 0.1−1 M⊙ yr−1
. Our search finds no candidates
at 15 < z < 20, placing upper limits at these redshifts. We develop a forward modeling approach to
infer the properties of the evolving luminosity function without binning in redshift or luminosity that
marginalizes over the photometric redshift uncertainty of our candidate galaxies and incorporates the
impact of non-detections. We find a z = 12 luminosity function in good agreement with prior results,
and that the luminosity function normalization and UV luminosity density decline by a factor of ∼ 2.5
from z = 12 to z = 14. We discuss the possible implications of our results in the context of theoretical
models for evolution of the dark matter halo mass function.
THE IMPORTANCE OF MARTIAN ATMOSPHERE SAMPLE RETURN.Sérgio Sacani
The return of a sample of near-surface atmosphere from Mars would facilitate answers to several first-order science questions surrounding the formation and evolution of the planet. One of the important aspects of terrestrial planet formation in general is the role that primary atmospheres played in influencing the chemistry and structure of the planets and their antecedents. Studies of the martian atmosphere can be used to investigate the role of a primary atmosphere in its history. Atmosphere samples would also inform our understanding of the near-surface chemistry of the planet, and ultimately the prospects for life. High-precision isotopic analyses of constituent gases are needed to address these questions, requiring that the analyses are made on returned samples rather than in situ.
Multi-source connectivity as the driver of solar wind variability in the heli...Sérgio Sacani
The ambient solar wind that flls the heliosphere originates from multiple
sources in the solar corona and is highly structured. It is often described
as high-speed, relatively homogeneous, plasma streams from coronal
holes and slow-speed, highly variable, streams whose source regions are
under debate. A key goal of ESA/NASA’s Solar Orbiter mission is to identify
solar wind sources and understand what drives the complexity seen in the
heliosphere. By combining magnetic feld modelling and spectroscopic
techniques with high-resolution observations and measurements, we show
that the solar wind variability detected in situ by Solar Orbiter in March
2022 is driven by spatio-temporal changes in the magnetic connectivity to
multiple sources in the solar atmosphere. The magnetic feld footpoints
connected to the spacecraft moved from the boundaries of a coronal hole
to one active region (12961) and then across to another region (12957). This
is refected in the in situ measurements, which show the transition from fast
to highly Alfvénic then to slow solar wind that is disrupted by the arrival of
a coronal mass ejection. Our results describe solar wind variability at 0.5 au
but are applicable to near-Earth observatories.
Gliese 12 b: A Temperate Earth-sized Planet at 12 pc Ideal for Atmospheric Tr...Sérgio Sacani
Recent discoveries of Earth-sized planets transiting nearby M dwarfs have made it possible to characterize the
atmospheres of terrestrial planets via follow-up spectroscopic observations. However, the number of such planets
receiving low insolation is still small, limiting our ability to understand the diversity of the atmospheric
composition and climates of temperate terrestrial planets. We report the discovery of an Earth-sized planet
transiting the nearby (12 pc) inactive M3.0 dwarf Gliese 12 (TOI-6251) with an orbital period (Porb) of 12.76 days.
The planet, Gliese 12 b, was initially identified as a candidate with an ambiguous Porb from TESS data. We
confirmed the transit signal and Porb using ground-based photometry with MuSCAT2 and MuSCAT3, and
validated the planetary nature of the signal using high-resolution images from Gemini/NIRI and Keck/NIRC2 as
well as radial velocity (RV) measurements from the InfraRed Doppler instrument on the Subaru 8.2 m telescope
and from CARMENES on the CAHA 3.5 m telescope. X-ray observations with XMM-Newton showed the host
star is inactive, with an X-ray-to-bolometric luminosity ratio of log 5.7 L L X bol » - . Joint analysis of the light
curves and RV measurements revealed that Gliese 12 b has a radius of 0.96 ± 0.05 R⊕,a3σ mass upper limit of
3.9 M⊕, and an equilibrium temperature of 315 ± 6 K assuming zero albedo. The transmission spectroscopy metric
(TSM) value of Gliese 12 b is close to the TSM values of the TRAPPIST-1 planets, adding Gliese 12 b to the small
list of potentially terrestrial, temperate planets amenable to atmospheric characterization with JWST.
Gliese 12 b, a temperate Earth-sized planet at 12 parsecs discovered with TES...Sérgio Sacani
We report on the discovery of Gliese 12 b, the nearest transiting temperate, Earth-sized planet found to date. Gliese 12 is a
bright (V = 12.6 mag, K = 7.8 mag) metal-poor M4V star only 12.162 ± 0.005 pc away from the Solar system with one of the
lowest stellar activity levels known for M-dwarfs. A planet candidate was detected by TESS based on only 3 transits in sectors
42, 43, and 57, with an ambiguity in the orbital period due to observational gaps. We performed follow-up transit observations
with CHEOPS and ground-based photometry with MINERVA-Australis, SPECULOOS, and Purple Mountain Observatory,
as well as further TESS observations in sector 70. We statistically validate Gliese 12 b as a planet with an orbital period of
12.76144 ± 0.00006 d and a radius of 1.0 ± 0.1 R⊕, resulting in an equilibrium temperature of ∼315 K. Gliese 12 b has excellent
future prospects for precise mass measurement, which may inform how planetary internal structure is affected by the stellar
compositional environment. Gliese 12 b also represents one of the best targets to study whether Earth-like planets orbiting cool
stars can retain their atmospheres, a crucial step to advance our understanding of habitability on Earth and across the galaxy.
The importance of continents, oceans and plate tectonics for the evolution of...Sérgio Sacani
Within the uncertainties of involved astronomical and biological parameters, the Drake Equation
typically predicts that there should be many exoplanets in our galaxy hosting active, communicative
civilizations (ACCs). These optimistic calculations are however not supported by evidence, which is
often referred to as the Fermi Paradox. Here, we elaborate on this long-standing enigma by showing
the importance of planetary tectonic style for biological evolution. We summarize growing evidence
that a prolonged transition from Mesoproterozoic active single lid tectonics (1.6 to 1.0 Ga) to modern
plate tectonics occurred in the Neoproterozoic Era (1.0 to 0.541 Ga), which dramatically accelerated
emergence and evolution of complex species. We further suggest that both continents and oceans
are required for ACCs because early evolution of simple life must happen in water but late evolution
of advanced life capable of creating technology must happen on land. We resolve the Fermi Paradox
(1) by adding two additional terms to the Drake Equation: foc
(the fraction of habitable exoplanets
with significant continents and oceans) and fpt
(the fraction of habitable exoplanets with significant
continents and oceans that have had plate tectonics operating for at least 0.5 Ga); and (2) by
demonstrating that the product of foc
and fpt
is very small (< 0.00003–0.002). We propose that the lack
of evidence for ACCs reflects the scarcity of long-lived plate tectonics and/or continents and oceans on
exoplanets with primitive life.
A Giant Impact Origin for the First Subduction on EarthSérgio Sacani
Hadean zircons provide a potential record of Earth's earliest subduction 4.3 billion years ago. Itremains enigmatic how subduction could be initiated so soon after the presumably Moon‐forming giant impact(MGI). Earlier studies found an increase in Earth's core‐mantle boundary (CMB) temperature due to theaccumulation of the impactor's core, and our recent work shows Earth's lower mantle remains largely solid, withsome of the impactor's mantle potentially surviving as the large low‐shear velocity provinces (LLSVPs). Here,we show that a hot post‐impact CMB drives the initiation of strong mantle plumes that can induce subductioninitiation ∼200 Myr after the MGI. 2D and 3D thermomechanical computations show that a high CMBtemperature is the primary factor triggering early subduction, with enrichment of heat‐producing elements inLLSVPs as another potential factor. The models link the earliest subduction to the MGI with implications forunderstanding the diverse tectonic regimes of rocky planets.
Climate extremes likely to drive land mammal extinction during next supercont...Sérgio Sacani
Mammals have dominated Earth for approximately 55 Myr thanks to their
adaptations and resilience to warming and cooling during the Cenozoic. All
life will eventually perish in a runaway greenhouse once absorbed solar
radiation exceeds the emission of thermal radiation in several billions of
years. However, conditions rendering the Earth naturally inhospitable to
mammals may develop sooner because of long-term processes linked to
plate tectonics (short-term perturbations are not considered here). In
~250 Myr, all continents will converge to form Earth’s next supercontinent,
Pangea Ultima. A natural consequence of the creation and decay of Pangea
Ultima will be extremes in pCO2 due to changes in volcanic rifting and
outgassing. Here we show that increased pCO2, solar energy (F⨀;
approximately +2.5% W m−2 greater than today) and continentality (larger
range in temperatures away from the ocean) lead to increasing warming
hostile to mammalian life. We assess their impact on mammalian
physiological limits (dry bulb, wet bulb and Humidex heat stress indicators)
as well as a planetary habitability index. Given mammals’ continued survival,
predicted background pCO2 levels of 410–816 ppm combined with increased
F⨀ will probably lead to a climate tipping point and their mass extinction.
The results also highlight how global landmass configuration, pCO2 and F⨀
play a critical role in planetary habitability.
Climate extremes likely to drive land mammal extinction during next supercont...
The stellar content_of_the_ring_in_ngc660
1. Astronomy & Astrophysics manuscript no. 0080 February 2, 2008
(DOI: will be inserted by hand later)
The stellar content of the ring in NGC 660 ⋆
G.M. Karataeva1,3 , N.A. Tikhonov2,4 , O.A. Galazutdinova2,4 , V.A. Hagen-Thorn1,3 , and V.A. Yakovleva1,3
1
Astronomical Institute, St.Petersburg State University, Universitetsky pr., 28, Petrodvoretz, St.Petersburg,
198504, Russia
2
Special Astrophysical Observatory, N.Arkhyz, Karachai-Circassian Rep., 369167, Russia
arXiv:astro-ph/0404286v1 14 Apr 2004
3
Isaac Newton Institute of Chile, St.Petersburg Branch
4
Isaac Newton Institute of Chile, SAO Branch
Received 15 January 2004 / Accepted 27 February 2004
Abstract. We present the results of stellar photometry of the polar-ring galaxy NGC 660 using the Hubble Space
Telescope’s archival data obtained with the Wide Field Planetary Camera 2. The final list of the resolved stars
contains 550 objects, a considerable part of which are blue and red supergiants belonging to the polar ring. The
analysis of the Colour Magnitude Diagram for polar ring stars shows that it is best represented by the isochrones
with metallicity Z = 0.008. The process of star formation in the polar ring was continuous and the age of the
youngest detected stars is about 7 Myr.
Key words. galaxies: individual: NGC 660 — galaxies: peculiar — galaxies: starburst — galaxies: stellar content
1. Introduction (Young et al., 1988; Armus et al. , 1990) observed in the
ring and the high mass of molecular gas sufficient for active
NGC 660, known for a long time as a peculiar galaxy con- star formation (Combes et al., 1992) may point to more
taining two inclined dust lanes (Benvenuti et al., 1976), recent star formation. Detecting blue supergiants in the
was included by Whitmore et al. (1990) in their catalogue ring may confirm this suggestion.
of Polar-Ring Galaxies (PRGs), candidates and related The galaxy is one of the nearest PRGs (D∼ 13 Mpc,
objects as a possible candidate (C - 13). The existence of H0 =75 km/s/Mpc) and resolving its ring into stars prob-
two different kinematic systems was established from radio ably may be achieved using HST images. Our study of
Hi (Gottesman & Mahon, 1990) and CO (Combes et al., PRGs NGC 2685 and NGC 4650A whose distances are fur-
1992) observations, and the galaxy was classified as a kine- ther than NGC 660 confirms this possibility (Karataeva
matically confirmed PRG (Arnaboldi & Galletta , 1993). et al., 2004, Paper I). The HST archive contains several
An extensive study of NGC 660 was performed by images of NGC 660, unfortunately not very deep. These
van Driel et al. (1995). The authors give a detailed de- images form the observational basis for our work devoted
scription of the host galaxy (which is spiral, while host to resolving the ring of the galaxy into stars.
galaxies in PRGs are usually lenticular or elliptical) and
its ring, which is not polar but is inclined to the disc
of the host galaxy by 55◦ . The authors notice that the 2. Observations and basic data processing
ring is very massive and may be stable (Sparke , 1986). We use archival HST/WFPC2 data of NGC 660 (see
Multicolour optical observations made with Schmidt tele- Table 1). These observations were carried out as part of
′′
scope with low resolution (5. 5) show that the ring is blue Proposals N 9042 and N 5446. The data set consists of
m
(V − Ic = 1. 0). From comparison with models of sin- images F 450W , F 814W , F 660W -bands with total expo-
gle burst star formation, the authors claim that the age sure times of 460 sec, 460 sec and 160 sec accordingly.
of the ring is about 2 Gyr. However, many Hii regions Unfortunately, these images cover only a part of the ring
(see Fig. 1). The total size of NGC 660 according to RC3 is
Send offprint requests to: G. Karataeva; e-mail: ′ ′
narka@astro.spbu.ru
8. 3 × 3. 2. At the distance of NGC 660 the scale is ≃ 65 pc
′′
⋆
Based on observations made with the NASA/ESA Hubble in 1 .
Space Telescope, obtained from the Space Telescope Science The raw frames were processed with the standard
Institute, which is operated by the Association of Universities WFPC2 pipeline. The data were extracted from the
for Research in Astronomy, Inc., under NASA contract NAS5- Archive using the On-The-Fly Reprocessing (OTFR)
26555. STScI archive system, which reconstructs and calibrates
2. 2 Karataeva et al.: The Stellar Content of NGC 660
Fig. 2. Completeness levels (left) and errors (right) of the
WFPC2 photometry.
m
24. 0 in Ic -band. Figure 2,right illustrates the precision of
our photometry.
Fig. 1. DSS2 8′ × 11′ image of NGC 660 with WFPC2
footprint overlaid. 3. Results
Table 1. Observation log The results of stellar photometry in the galaxy NGC 660
obtained after correcting for absorption in our Galaxy
m m m
(AB = 0. 28, AV = 0. 21, AIc = 0. 12 (Schlegel et al.,
Date Band Exposure 1998)) are presented in Colour–Magnitude Diagrams
(CMDs) in Fig. 3. For the CMD B vs. (B − Ic ) there is a
04.07.1995 F660w 2 × 80sec concentration of blue stars in the region 0 < (B − Ic ) <
03.07.2001 F450w 2 × 230sec m m m
1. 0 and 23. 0 < B < 25. 0. Taking into account that there
F814w 2 × 230sec must be intrinsic absorption in NGC 660 these stars may
be considered as blue supergiants by their colour indexes
and luminosities (for NGC 660 the distance modulus is
the original data with the latest calibration files, soft- m
m-M =30. 6). The bulk of them are located in the region
ware and data parameters. For details of the processing of the polar ring (Fig. 4).
see Paper I. While blue supergiants are detected in the CMD B
The single-star photometry of the images was pro- vs. (B − Ic ) quite reliably (the normal position for blue
cessed with DAOPHOT/ALLSTAR. These programs use auto- supergiants can be found from Bertelli et al. (1994)), the
matic star-finding algorithms and then measure the stel- red supergiants, being near the limit in the F 450W image,
lar magnitude by fitting a PSF that is constructed from are somewhat uncertainly. Nevertheless, some stars with
the stars in uncrowded parts of the images. Then we de- m m m
B < 25. 5 and 2. 8 < (B − Ic ) < 4. 0 are located in the
termined the aperture correction from the 1.5 pixel ra- ring. The F 660W image is more favorable for detecting
′′
dius aperture to the standard 0. 5 radius aperture size red supergiants. Unfortunately, only a small part of the
for the WFPC2 photometric system using bright un- stars of the ring and host galaxy are represented in the
crowded stars. The F 450W , F 606W and F 814W instru- CMD Ic vs. (V − Ic ) (Fig. 3, right) because of the very
mental magnitudes were transformed to standard BV Ic short exposure time of the image as well as the large shift
in the Johnson-Cousins system using the prescriptions between the F 660W and F 814W images. However, one
of Holtzman et al. (1995). Background galaxies, unre- can see a concentration of stars in the region where red
solved blends and stars contaminated by cosmetic CCD m m
supergiants may be located (Ic ≈ 22. 5 and V −Ic ≈ 2. 0).
blemishes which have “quality” parameters as defined in A part of these stars are located in the ring.
ALLSTAR in MIDAS |SHARP | > 0.1, |CHI| > 1.0 were In Fig. 5,left we give the observed CMD MIc vs (B −Ic )
eliminate from the final list which contains 550 stars. for all resolved stars constructed with the distance mod-
m
The results of the artificial star completeness test are ulus m-M =30. 6. Absolute magnitudes of the blue stars
shown in Fig. 2,left. The recovery is practically complete are normal for blue supergiants, and taking into account
m m
up to m = 23. 5 in B-band , m = 23. 5 in V -band and m = their positions (Fig. 4) we have no reason not to consider
3. Karataeva et al.: The Stellar Content of NGC 660 3
Fig. 3. Colour–Magnitude Diagrams B vs. (B − Ic ) (left) and Ic vs. (V − Ic ) (right) corrected for absorption in our
Galaxy.
Fig. 4. WFPC2 image of NGC 660. Left: circles and squares indicate the position of blue and red supergiants, cor-
respondingly. The stars located inside the ellipse were rejected in construction of Fig. 5, right. Right: two stellar
complexes in the enlarged part (box on the left) of the NGC 660 polar ring.
them as ring stars. This is confirmed, in particular, by therein (van Driel et al., 1995). The dust is seen directly
the location of some stars in complexes, two of which are as a dark strip in the region where the ring is projected
presented in Fig. 4,right. One may expect that these com- on the disc of the galaxy. The dusty nature of the strip
plexes contain young stars. Such complexes were found in is confirmed by polarimetry (Reshetnikov & Yakovleva ,
polar rings of the galaxies NGC 2685 and NGC 4650A 1991; Alton et al., 2000).
(PaperI). In the latter paper it is found that the absorption of
m
The large width of the blue supergiants branch (0 < the light of galactic disc by the ring is equal to 1. 2 in
−τv
(B − Ic ) < 1) in Fig. 3,left and Fig. 5,left may be ex- the V - band (i.e. because AV = −2.5 lg e the opti-
plained by the different intrinsic absorption of various cal depth of dust layers in the ring is τv = 1.1). This
stars. The presence of dust in the ring may be expected value gives the upper limit of absorption for the ring
from the large amount of neutral hydrogen observed stars. Having no possibility to correct for absorption mag-
4. 4 Karataeva et al.: The Stellar Content of NGC 660
Fig. 5. MIc vs (B − Ic ) CMDs of NGC 660: left – for all resolved stars; right – for ring stars after correction for
intrinsic absorption in the ring. Stellar isochrones for the metallicity Z=0.008 from the Padova library are overplotted.
Dashed line on the right represents an example of a stellar isochrone for the metallicity Z=0.02.
nitudes and colour indexes of each star individually we was found for NGC 2685 (PaperI) and some other po-
correct CMDs for intrinsic absorption on average. If in lar rings (Radtke et al. , 2003). This is an important fact
the ring the dust and stars are mixed then for τv = 1.1 which should be taken into account in choosing a scenario
one can find (Disney et al. , 1989) the mean absorption of polar ring formation.
m
for the ring stars of 0. 54. For a normal reddening curve Fig. 5,right shows that in the ring of NGC 660 there
m m
(Cardelli et al. , 1989) this gives AB = 0. 69, AIc = 0. 34, are very young stars with ages 7÷9 Myr. Grouping the
m m
E(B−Ic ) = 0. 35 and E(V−Ic ) = 0. 22. These values may stars in complexes (see Fig. 4,right) shows that the stars
be used to correct CMDs. are not yet dispersed in the stellar field, confirming their
Because our goal is to investigate the stellar content youth.
of the ring we should eliminate the stars not belonging to Because the CMD in Fig. 5,right is not deep, we can-
it from the final diagram. The final CMD for polar ring not conclude anything about age of the ring. It may also
stars after correcting for intrinsic absorption and eliminat- contain old stars, like the Arp ring near M 81, where
ing stars of the host galaxy (made geometrically, as shown Tikhonov & Galazutdinova (2004) detected red giants as
in Fig. 4,left) is given in Fig. 5,right. Note that there is well as young blue stars.
only a small difference between features in Figs. 5,right The relative youth of the ring is confirmed by
and left in the region of blue stars, which, therefore, be- its blue colour, as derived from surface photometry.
long to the ring. Of course, the CMD may contain some van Driel et al. (1995) showed that the ring with its colour
contaminating objects from our Galaxy (for instance, the m
index V − Ic ≈ 1. 0 is much bluer than the galaxy disc.
m m
object which has MIc ≈ −10. 8 and B − Ic ≈ 2. 6), but Dividing frame F 450W by frame F 814W (see Fig. 6) con-
their number is not large. firms this. By comparison of this colour index with models
of galactic colour evolution, van Driel et al. (1995) found
that the age of the ring is about 2×109 years. However,
4. Discussion
the authors did not take into account any reddening.
The CMD for ring stars (Fig. 5,right) may be used for Alton et al. (2000) corroborated this and found that after
estimation of their ages and metallicity by comparison correcting for intrinsic absorption (which they somewhat
m
with calculated isochrones. Bertelli et al. (1994) provide overestimated) the colour-index reduces to V − Ic ≈ 0. 7
8
these isochrones for various metallicities. In Fig. 5,right and age – to ∼ 10 years (this value was found after an
isochrones for the metallicity Z=0.008 are overplotted on incorrect comparison of the colour index V − Ic (Cousins)
the CMD. Although the number of red supergiants is with models, calculated for V − I (Johnson)). Indeed, the
m
small, they allow us to choose between the isochrones full (Galactic and intrinsic) colour excess is EV−Ic = 0. 31
with different metallicity . The isochrones for the metallic- (see above) and correct comparison with the models cal-
ity Z=0.008 are in the best agreement with the observed culated for V − Ic (Cousins) (Kurth et al., 1999) give the
CMD. The isochrones for higher metallicity (for exam- age of the ring as 1×109 years.
ple, solar, Z=0.02) contradict with the observed CMD (see A final conclusion about the age of the ring may be ob-
Fig. 5,right) . A relatively low metallicity in the polar rings tained only after constructing the CMD sufficiently deep
5. Karataeva et al.: The Stellar Content of NGC 660 5
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7÷9 Myr. The relatively low metallicity of these stars is in Cameron T.Y.,Sackett P.D., Olling R.P. 1990, AJ, 100,
accordance with the data for polar rings in other PRGs. 1489
It is very important to reach the region of red Young J.S., Kleinmann S.G., & Allen L.E., 1988, ApJ,
giants in CMDs. This might give not only the in- 334, L63
formation about ring age but also assist in choosing
the model of ring formation because the merging sce-
nario (Bournaud & Combes, 2003) predicts the existence
around the galaxy of a halo from old/intermediate age
stars. Longer exposures with HST may allow us to con-
struct such CMDs.
Acknowledgements. This work was supported by RFBR via
grants 03-02-16344 and 02-02-16033.
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