The muse 3_d_view_of_the_hubble_deep_field_southSérgio Sacani
Artigo mostra como foram as observações feitas com o MUSE, o novo instrumento do VLT do campo profundo do Hubble. Além de descobrir 20 novos objetos, o MUSE conseguiu medir as propriedades das galáxias e até representar as mais próximas em 3 dimensões.
The muse 3_d_view_of_the_hubble_deep_field_southSérgio Sacani
Artigo mostra como foram as observações feitas com o MUSE, o novo instrumento do VLT do campo profundo do Hubble. Além de descobrir 20 novos objetos, o MUSE conseguiu medir as propriedades das galáxias e até representar as mais próximas em 3 dimensões.
tells about history,physics of remote sensing,electromagnetic spectrum,black body radiation,atmospheric windows,interaction of EMR with atmosphere,earth surface features,spectral reflectance curves
hyperspectral remote sensing and its geological applicationsabhijeet_banerjee
this is an introductory presentation on hyperspectral remote sensing, which essential deals with the distinguishing features, imaging spectrometers and its types, and some of the geological applications of hyperspectral remote sensing.
tells about history,physics of remote sensing,electromagnetic spectrum,black body radiation,atmospheric windows,interaction of EMR with atmosphere,earth surface features,spectral reflectance curves
hyperspectral remote sensing and its geological applicationsabhijeet_banerjee
this is an introductory presentation on hyperspectral remote sensing, which essential deals with the distinguishing features, imaging spectrometers and its types, and some of the geological applications of hyperspectral remote sensing.
GOALS-JWST: Unveiling Dusty Compact Sources in the Merging Galaxy IIZw096Sérgio Sacani
We have used the Mid-InfraRed Instrument (MIRI) on the James Webb Space Telescope (JWST) to obtain the first
spatially resolved, mid-infrared images of IIZw096, a merging luminous infrared galaxy (LIRG) at z = 0.036.
Previous observations with the Spitzer Space Telescope suggested that the vast majority of the total IR luminosity
(LIR) of the system originated from a small region outside of the two merging nuclei. New observations with
JWST/MIRI now allow an accurate measurement of the location and luminosity density of the source that is
responsible for the bulk of the IR emission. We estimate that 40%–70% of the IR bolometric luminosity, or
3–5 × 1011 Le, arises from a source no larger than 175 pc in radius, suggesting a luminosity density of at least
3–5 × 1012 Le kpc−2
. In addition, we detect 11 other star-forming sources, five of which were previously
unknown. The MIRI F1500W/F560W colors of most of these sources, including the source responsible for the
bulk of the far-IR emission, are much redder than the nuclei of local LIRGs. These observations reveal the power
of JWST to disentangle the complex regions at the hearts of merging, dusty galaxies.
High-resolution UV/Optical/IR Imaging of Jupiter in 2016–2019Sérgio Sacani
Imaging observations of Jupiter with high spatial resolution were acquired beginning in 2016, with a cadence of 53
days to coincide with atmospheric observations of the Juno spacecraft during each perijove pass. The Wide Field
Camera 3 (WFC3) aboard the Hubble Space Telescope (HST) collected Jupiter images from 236 to 925 nm in 14
filters. The Near-Infrared Imager (NIRI) at Gemini North imaged Jovian thermal emission using a lucky-imaging
approach (co-adding the sharpest frames taken from a sequence of short exposures), using the M′ filter at 4.7 μm.
We discuss the data acquisition and processing and an archive collection that contains the processed WFC3 and
NIRI data (doi:10.17909/T94T1H). Zonal winds remain steady over time at most latitudes, but significant
evolution of the wind profile near 24°N in 2016 and near 15°S in 2017 was linked with convective superstorm
eruptions. Persistent mesoscale waves were seen throughout the 2016–2019 period. We link groups of lightning
flashes observed by the Juno team with water clouds in a large convective plume near 15°S and in cyclones near
35°N–55°N. Thermal infrared maps at the 10.8 micron wavelength obtained at the Very Large Telescope show
consistent high brightness temperature anomalies, despite a diversity of aerosol properties seen in the HST data.
Both WFC3 and NIRI imaging reveal depleted aerosols consistent with downwelling around the periphery of the
15°S storm, which was also observed by the Atacama Large Millimeter/submillimeter Array. NIRI imaging of
the Great Red Spot shows that locally reduced cloud opacity is responsible for dark features within the vortex. The
HST data maps multiple concentric polar hoods of high-latitude hazes.
First results from_the_hubble_opal_program_jupiter_in_2015Sérgio Sacani
Os cientistas usando o Telescópio Espacial Hubble da NASA/ESA produziram novos mapas de Júpiter, que mostram as contínuas mudanças que ocorrem com a famosa Grande Mancha Vermelha. As imagens também revelam uma rara estrutura em forma de onda na atmosfera do planeta que não tinha sido vista por décadas. A nova imagem é a primeira de uma série de retratos anuais dos planetas externos do Sistema Solar, que nos darão um novo olhar desses mundos remotos, e ajudarão os cientistas a estudarem como eles mudam com o passar do tempo.
Nessa nova imagem de Júpiter, uma grande quantidade de feições foi capturada incluindo ventos, nuvens e tempestades. Os cientistas por trás dessas novas imagens, as obtiveram usando a Wide Field Camera 3 do Hubble, num período de observação de mais de 10 horas e produziram assim dois mapas completos do planeta, a partir das suas observações. Esses mapas fizeram com que fosse possível determinar a velocidade dos ventos em Júpiter, com a finalidade de identificar diferentes fenômenos na sua atmosfera além de traquear as suas feições mais famosas.
As novas imagens confirmam que a grande tempestade que tem existido na superfície de nuvens de Júpiter por no mínimo 300 anos, continua a encolher, mas mesmo que desapareça, ela irá morrer lutando. A tempestade, conhecida como Grande Mancha Vermelha, é vista aqui fazendo seus movimentos em espiral no centro da imagem do planeta. Ela tem diminuído de tamanho de maneira muito rápida de ano em ano. Mas agora, a taxa de encolhimento parece ter reduzido novamente, mesmo apesar da mancha ser cerca de 240 quilômetros menor do que era em 2014.
Beyond the disk: EUV coronagraphic observations of the Extreme Ultraviolet Im...Sérgio Sacani
Most observations of the solar corona beyond 2 R consist of broadband visible light imagery carried out with coronagraphs.
The associated diagnostics mainly consist of kinematics and derivations of the electron number density. While the measurement of the
properties of emission lines can provide crucial additional diagnostics of the coronal plasma (temperatures, velocities, abundances,
etc.), these types of observations are comparatively rare. In visible wavelengths, observations at these heights are limited to total
eclipses. In the ultraviolet (UV) to extreme UV (EUV) range, very few additional observations have been achieved since the pioneering
results of the Ultraviolet Coronagraph Spectrometer (UVCS).
Aims. One of the objectives of the Full Sun Imager (FSI) channel of the Extreme Ultraviolet Imager (EUI) on board the Solar Orbiter
mission has been to provide very wide field-of-view EUV diagnostics of the morphology and dynamics of the solar atmosphere in
temperature regimes that are typical of the lower transition region and of the corona.
Methods. FSI carries out observations in two narrowbands of the EUV spectrum centered on 17.4 nm and 30.4 nm that are dominated,
respectively, by lines of Fe ix/x (formed in the corona around 1 MK) and by the resonance line of He ii (formed around 80 kK in the
lower transition region). Unlike previous EUV imagers, FSI includes a moveable occulting disk that can be inserted in the optical path
to reduce the amount of instrumental stray light to a minimum.
Results. FSI detects signals at 17.4 nm up to the edge of its field of view (7 R), which is about twice further than was previously
possible. Operation at 30.4 nm are for the moment compromised by an as-yet unidentified source of stray light. Comparisons with
observations by the LASCO and Metis coronagraphs confirm the presence of morphological similarities and differences between the
broadband visible light and EUV emissions, as documented on the basis of prior eclipse and space-based observations.
Conclusions. The very-wide-field observations of FSI out to about 3 and 7 R, without and with the occulting disk, respectively, are
paving the way for future dedicated instruments.
Dr. Kent Miller presents an overview of his program, Space Science, at the AFOSR 2013 Spring Review. At this review, Program Officers from AFOSR Technical Divisions will present briefings that highlight basic research programs beneficial to the Air Force.
First Observation of the Earth’s Permanent FreeOscillation s on Ocean Bottom ...Sérgio Sacani
The Earth’s hum is the permanent free oscillations of the Earth recorded in the absence ofearthquakes, at periods above 30 s. We present the first observations of its fundamental spheroidaleigenmodes on broadband ocean bottom seismometers (OBSs) in the Indian Ocean. At the ocean bottom,the effects of ocean infragravity waves (compliance) and seafloor currents (tilt) overshadow the hum. In ourexperiment, data are also affected by electronic glitches. We remove these signals from the seismic traceby subtracting average glitch signals; performing a linear regression; and using frequency-dependentresponse functions between pressure, horizontal, and vertical seismic components. This reduces the longperiod noise on the OBS to the level of a good land station. Finally, by windowing the autocorrelation toinclude only the direct arrival, the first and second orbits around the Earth, and by calculating its Fouriertransform, we clearly observe the eigenmodes at the ocean bottom.
Measurements of the_near_nucleus_coma_of_comet_67_p_churyumov_gerasimenko_wit...Sérgio Sacani
Artigo descreve descoberta feita pelo instrumento Alice da sonda Rosetta no cometa 67P/Churyumov-Gerasimenko, das moléculas de água e dióxido de carbono quebradas que pairam pela atmosfera do cometa.
Simulation of the Earth’s radio-leakage from mobile towers as seen from selec...Sérgio Sacani
Mobile communication towers represent a relatively new but growing contributor to the total radio leakage associated with
planet Earth. We investigate the overall power contribution of mobile communication towers to the Earth’s radio leakage budget,
as seen from a selection of different nearby stellar systems. We created a model of this leakage using publicly available data of
mobile tower locations. The model grids the surface of the planet into small, computationally manageable regions, assuming
a simple integrated transmission pattern for the mobile antennas. In this model, these mobile tower regions rise and set as the
Earth rotates. In this way, a dynamic power spectrum of the Earth was determined, summed over all cellular frequency bands.
We calculated this dynamic power spectrum from three different viewing points - HD 95735, Barnard’s star, and Alpha Centauri
A. Our preliminary results demonstrate that the peak power leaking into space from mobile towers is ∼ 4GW. This is associated
with LTE mobile tower technology emanating from the East Coast of China as viewed from HD 95735. We demonstrate that
the mobile tower leakage is periodic, direction dependent, and could not currently be detected by a nearby civilisation located
within 10 light years of the Earth, using instrumentation with a sensitivity similar to the Green Bank Telescope (GBT). We plan
to extend our model to include more powerful 5G mobile systems, radar installations, ground based up-links (including the Deep
Space Network), and various types of satellite services, including low-Earth orbit constellations such as Starlink and OneWeb.
Terra Seismic can predict most major earthquakes (M6.2 or greater) at least 2 - 5 months before they will strike. Global earthquake prediction is based on determinations of the stressed areas that will start to behave abnormally before
major earthquakes. The size of the observed stressed areas roughly corresponds to estimates calculated from Dobrovolsky’s formula. To identify abnormalities and make predictions, Terra Seismic applies various methodologies, including satellite remote sensing methods and data from ground-based
instruments. We currently process terabytes of information daily, and use more than 80 different multiparameter prediction systems. Alerts are issued if the abnormalities are confirmed by at least five different systems. We observed that geophysical patterns of earthquake development and stress accumulation
are generally the same for all key seismic regions. Thus, the same earthquake prediction methodologies and systems can be applied successfully worldwide. Our technology has been used to retrospectively test data gathered since 1970 and it successfully detected about 90 percent of all significant quakes over the last 50 years.
An elevation of 0.1 light-seconds for the optical jet base in an accreting Ga...Sérgio Sacani
Relativistic plasma jets are observed in many systems that
host accreting black holes. According to theory, coiled magnetic
fields close to the black hole accelerate and collimate the
plasma, leading to a jet being launched1–3. Isolating emission
from this acceleration and collimation zone is key to measuring
its size and understanding jet formation physics. But this
is challenging because emission from the jet base cannot
easily be disentangled from other accreting components. Here,
we show that rapid optical flux variations from an accreting
Galactic black-hole binary are delayed with respect to X-rays
radiated from close to the black hole by about 0.1 seconds, and
that this delayed signal appears together with a brightening
radio jet. The origin of these subsecond optical variations
has hitherto been controversial4–8. Not only does our work
strongly support a jet origin for the optical variations but it
also sets a characteristic elevation of ≲ 103 Schwarzschild
radii for the main inner optical emission zone above the black
hole9, constraining both internal shock10 and magnetohydrodynamic11
models. Similarities with blazars12,13 suggest that jet
structure and launching physics could potentially be unified
under mass-invariant models. Two of the best-studied jetted
black-hole binaries show very similar optical lags8,14,15, so this
size scale may be a defining feature of such systems.
The internal structure_of_asteroid_itokawa_as_revealed_by_detection_of_yorp_s...
FINAL
1. The Radio Eyes: Observing the Sun, Jupiter and IO
Nathan Sharifrazi, Megan Naghibian, Taylor Patti
2014 Summer Undergraduate Research
Schmid College of Science and Technology, Chapman University, Orange, CA
Mentor: Eric Minassian, PhD
Introduction
The purpose of this research was to develop
practical intuition and gain firsthand experience in
radio astronomy. Radio Waves form a major
component of the Electromagnetic Spectrum (Figure
1), which also contains microwaves and visible light.
Our atmosphere is opaque to most EM waves,
but there are windows of transparency both in visible
and radio range.
By constructing and implementing four Radio
receivers and antennas, the SuperSID, INSPIRE,
IBT, and Radio JOVE we were able to intercept
Radio Waves in the transparent region from
astronomical and man-made sources alike, enabling
us to attain data on the behavior of the Sun,
terrestrial weather, the planet Jupiter, and Jupiter's
moon itself, respectively.
Hypothesis
The universe being rich in Radio length
Electromagnetic Radiation, these Radio telescopes
will intercept ample radiation from various
astronomical and terrestrial sources, thus providing
for a greater insight and understanding of many
natural phenomena not easily studied by other
methods.
Figure 1. The Electromagnetic Spectrum
INSPIRE
A receiver and a virtual dipole antenna (ten-feet
monopole + a virtual mirror image in the ground), the
INSPIRE is an extremely sensitive apparatus which cannot
be within 500 meters of even the most modest of modern
electronics, this device provides information on the
duration of various terrestrial weather events, with special
emphasis on lightning and thunderstorms.
Figure 3. SuperSID July 28, 2014 report corresponding to spaceweather.com
Rapid bursts of high intensity and short duration were
detected by the Radio JOVE (Figure 6). The associated
audio files yielded rapid popping noises known as S-
bursts.
S-bursts are caused by storms on Jupiter associated
with its moon IO. These bursts are rapid and plentiful,
occurring at a fairly high frequency and creating a popping
sounds on the audio output of the receiver, much like the
experimental data collected in this project (2). Moreover,
observations from other Radio Astronomers taken from
NASA’s corresponding support page agrees with this
findings, indicating that these types of storms were
detected on Jupiter within a 24 hour period of these
observations (5).
Future Research
Each of these apparatuses provides foundation for
nearly limitless application and study. While in
subsequent experiments the versatile IBT could be
employed in detecting emissions from far-off stars and
galaxies and locating and tracking the movement of
satellites and even humans, the powerful Radio JOVE
can provide detailed information on the activities of the
Sun, Jupiter and Jupiter's moon IO. Moreover, just as the
SuperSID can be utilized to compile extensive data on
sunspot activities and ultimately achieve a greater
understanding of solar weather patterns, the INSPIRE
project can furnish information with regards to terrestrial
weather, including the generation and patterns of
thunderstorms on Earth.
References
(1) Bennett, R., (2007). The INSPIRE VLF-3 RECEIVER Theory of
Operation. Retrieved from
http://image.gsfc.nasa.gov/poetry/inspire/2007/RSPublication/Theory_of_Operations.pdf.
(2)Flagg, R.S., (2012). JOVE RJ1.1 Receiver Kit Assembly Manual. Retrieved from
http://radiojove.gsfc.nasa.gov/telescope/rcvr_manual.pdf.
(3)Phillips, T., (2010). Space Weather Conditions. Retrieved from
http://spaceweather.com/archive.php?view=1&day=28&month=07&year=2014.
(4) Scherrer, D., Mitchell, R., et al. (2009). Sudden Ionospheric Disturbance Space
Weather Monitor Manual. Retrieved from http://solar-
center.stanford.edu/SID/Distribution/SuperSID/supersid_v1_1/Doc/SuperSIDManual_v1.p
df.
(5) Typinski, D., (2014) Radio JOVE Data Archived Display. Retrieved from
http://radiojove.org/cgi-
bin/rjdisplay.pl?sortdate1=201408070000&sortdate2=201408070000&STRING=
Jupiter.
(6)Young, H.D., Freedman, R., et al. (2013). University Physics with
Modern Physics Technology Update. San Francisco, CA: Pearson Addison-
Wesley.
The definitive and marked peaks during the daytime
hours indicate that solar flares were occurring during
those hours. This was corroborated by NASA’s Space
Weather report, which reported 110 sunspots developing
on that day (3).
IBT (Itty Bitty Telescope)
The IBT is a simple and dynamic device which is
constructed from a recycled cable television parabolic dish
and a basic satellite finder. Sensing SHF (Super High
Frequency) Radio waves, it senses blackbody radiation
and it enables the user to discern between bodies and
regions of various temperatures . In this project, the IBT
was mounted on a stand with a lazy-Suzanne design in
order to facilitate accurately observing various targets.
The IBT showed dramatic difference with solar vs.
“cold sky” regions. As (Figure 5) indicates, the thermal
intensity of the device increased nearly 7 times when the
antenna’s focus briefly panned past the sun.
The average temperatures of empty universe and the
Sun are 3 and 5,778 Kelvin respectively (6). This massive
temperature difference accounts for the seven to one
increase which occurred when the IBT was directed at the
Sun rather than at “cold sky”. Many factors such as noise
in the antenna and the environment accounts for this
difference.
CU1: Chapman University SuperSID Monitor
Observation: Date: 24-hr observation for Jul28, 2014. Location: Aliso Viejo, CA. Lat/long: 33°34'N / 117°44'W.
UTC = PDT +7 Sunrise on Jul28: 6:00 AM PDT (1:00 PM UTC). Sunset on Jul28: 7:54 PM PDT (2:54 AM, Next Day, UTC).
Observed: X-Ray Solar Flare, category C2 observed at 1410 UT Jul28, more prominent on NWC signal at 19,800 Hz
A category C1 X-ray solar flare occurred at 1930 UT Jul28 2014, but was not observed possibly due to lowering ionization at sunset
X-ray Solar Flare
Category C2 at 1410 UT
Jul28
Graphs
Station Frequency (Hz) Location Color
NWC 19800 Australia Blue
NPM 21400 HI, USA Green
JJI 22200 Japan Red
HWU 21750 France Yellow
The SuperSID
The concept and design of the SuperSID is a
small, transportable circuitry case attached to a loop
antenna of wire and wood; it detects the VLF (very
low frequency) Radio waves which are emitted by
naval bases around the world to communicate with
submarines(4).
By comparing the relative intensity of such waves
throughout the day, it monitors the status of the
Ionosphere, which is activated by solar radiation. In this
manner, sunspots and other solar activities can be
monitored through SID, CME (coronal Mass Ejections)
and mapped. Allowing for a -7 hour offset to correctly
convert the Universal Time Coordinate to local time
(Mission Viejo, CA), the SuperSID data (Figure 3) yields
intensity jumps significantly greater than typical daytime
observation with no solar activity.
Radio JOVE
Hours of careful soldering, diligent assembly, and
precise tuning culminated in the Radio Jove, a functioning
radio receiver that is used to monitor emissions from the
Sun, Jupiter, and Jupiter's moon IO. The Radio Jove
combines a complex circuitry with a massive dual dipole
up to 20 feet in height, 25 feet long and over 1,000 square
feet in cross sectional area.
The Inspire antenna provided a gentle cracking and
popping sound, which was adapted to a graph showing a
somewhat oscillatory pattern of rapid and continuous radio
emission.
Sferics are cracking and popping noises associated
with lightning strikes up to 3,000 kilometers away (1). A
graph of this is somewhat consistent with the data which
the Inspire device received, indicating the possibility of a
lightning strike within the 28 million square kilometers
surrounding the testing site (Orange, CA). However, the
experimental data oscillates somewhat more rapidly,
indicating that interference from power lines may have
been involved.
Figure 4. INSPIRE August 6, 2014 data.
Figure 5. IBT data August 2, 2014 panning over the Sun.
Figure 6. Radio JOVE August 4, 2014 data including tests disconnecting the
antenna from the receiver.
Figure 2. Atmospheric Opacity for EM waves