On the (Non-)Enhancment of the Lyα Equivalent Width by a Multiphase Interstel...Edmund Christian Herenz
Talk at MUSE Science Meeting @ Leibniz-Institut für Astrophysik in Potsdam (AIP) presenting a recent Paper by P. Laursen et al. http://dx.doi.org/10.1088/0004-637X/766/2/124
ESC Talk on the seminal paper from 1967 by Partidge & Peebles, where they predicted the visibilty of galaxies in the early universe by the virtue of their strong Lyman Alpha emission.
On the (Non-)Enhancment of the Lyα Equivalent Width by a Multiphase Interstel...Edmund Christian Herenz
Talk at MUSE Science Meeting @ Leibniz-Institut für Astrophysik in Potsdam (AIP) presenting a recent Paper by P. Laursen et al. http://dx.doi.org/10.1088/0004-637X/766/2/124
ESC Talk on the seminal paper from 1967 by Partidge & Peebles, where they predicted the visibilty of galaxies in the early universe by the virtue of their strong Lyman Alpha emission.
Superflares in G, K and M Type Dwarfs from Kepler ObservationsSimon Candelaresi
We study the occurrence of superflares in G, K and M type dwarfs from lightcurves obtained by the Kepler mission. From that set 380 stars are detected with flares above 10^34 erg with 1690 such events. Various stellar parameters are considered here to find what circumstances are favorable for the occurrence of superflares. With decreasing effective temperature the flaring rate increases, as well as with an increase in the star's rotation rate. Star spots, which are a proxy for the magnetic field strength and dynamo activity, are seen more frequently in flaring stars and cover a larger proportion of the star's. surface. Using Ohmic dissipation as proxy for flare events, we perform simulations for a turbulent dynamo and find an increase of Ohmic dissipation as the dynamo number increases, in line with the observations.
Fractional approaches in dielectric broadband spectroscopySimon Candelaresi
A fractional approach is used to describe data from dielectric spectroscopy for several glassy materials. Using composite fractional time evolution propagators a modified law for relaxation in glasses is found that describes the experimental data for broadband dielectric spectroscopy. Properties and solutions of some particular fractional differential equations (fDEQs) are investigated both for rational and irrational order. The laws of Debye, Kohlrausch, Cole-Cole, ColeDavidson and Havriliak-Negam
Using the inclinations_of_kepler_systems_to_prioritize_new_titius_bode_based_...Sérgio Sacani
Artigo descreve como cientistas aplicaram a relação de Titius-Bode nos dados do Kepler para prever a existência de bilhões de exoplanetas parecidos com a Terra na Via Láctea.
One of the key science cases for the 2nd generation VLT instrument
MUSE is the exploration of uncharted territories in the observable
parameter space of Lyman-alpha emitters at 3.1 < z < 6.5. In my talk
I will give a presentation of the instrument, highlighting its unique
capabilities in upcoming LAE surveys. I will then explain a method
based on matched filtering which can be used to identify LAE galaxies
in future datasets from this instrument. I will conclude by showing
results obtained from tests on simulated MUSE observations
demonstrating the reliability and robustness of this method.
Communiqué features articles focusing on the latest hot topics for anesthesiologists, nurse anesthetists, pain management specialists and anesthesia practice administrators.
Communique is created by Anesthesia Business Consultants (ABC), the largest physician billing and practice management company specializing exclusively in the practice of anesthesia and pain management.
ABC serves several thousand anesthesiologists and CRNAs nationwide with anesthesia billing software solutions.
Please send your email address to info [at] anesthesiallc [dot] com if you would like to join the Communique mailing list!
Visit www.anesthesiallc.com for more information!
Superflares in G, K and M Type Dwarfs from Kepler ObservationsSimon Candelaresi
We study the occurrence of superflares in G, K and M type dwarfs from lightcurves obtained by the Kepler mission. From that set 380 stars are detected with flares above 10^34 erg with 1690 such events. Various stellar parameters are considered here to find what circumstances are favorable for the occurrence of superflares. With decreasing effective temperature the flaring rate increases, as well as with an increase in the star's rotation rate. Star spots, which are a proxy for the magnetic field strength and dynamo activity, are seen more frequently in flaring stars and cover a larger proportion of the star's. surface. Using Ohmic dissipation as proxy for flare events, we perform simulations for a turbulent dynamo and find an increase of Ohmic dissipation as the dynamo number increases, in line with the observations.
Fractional approaches in dielectric broadband spectroscopySimon Candelaresi
A fractional approach is used to describe data from dielectric spectroscopy for several glassy materials. Using composite fractional time evolution propagators a modified law for relaxation in glasses is found that describes the experimental data for broadband dielectric spectroscopy. Properties and solutions of some particular fractional differential equations (fDEQs) are investigated both for rational and irrational order. The laws of Debye, Kohlrausch, Cole-Cole, ColeDavidson and Havriliak-Negam
Using the inclinations_of_kepler_systems_to_prioritize_new_titius_bode_based_...Sérgio Sacani
Artigo descreve como cientistas aplicaram a relação de Titius-Bode nos dados do Kepler para prever a existência de bilhões de exoplanetas parecidos com a Terra na Via Láctea.
One of the key science cases for the 2nd generation VLT instrument
MUSE is the exploration of uncharted territories in the observable
parameter space of Lyman-alpha emitters at 3.1 < z < 6.5. In my talk
I will give a presentation of the instrument, highlighting its unique
capabilities in upcoming LAE surveys. I will then explain a method
based on matched filtering which can be used to identify LAE galaxies
in future datasets from this instrument. I will conclude by showing
results obtained from tests on simulated MUSE observations
demonstrating the reliability and robustness of this method.
Communiqué features articles focusing on the latest hot topics for anesthesiologists, nurse anesthetists, pain management specialists and anesthesia practice administrators.
Communique is created by Anesthesia Business Consultants (ABC), the largest physician billing and practice management company specializing exclusively in the practice of anesthesia and pain management.
ABC serves several thousand anesthesiologists and CRNAs nationwide with anesthesia billing software solutions.
Please send your email address to info [at] anesthesiallc [dot] com if you would like to join the Communique mailing list!
Visit www.anesthesiallc.com for more information!
Communiqué features articles focusing on the latest hot topics for anesthesiologists, nurse anesthetists, pain management specialists and anesthesia practice administrators.
Communique is created by Anesthesia Business Consultants (ABC), the largest physician billing and practice management company specializing exclusively in the practice of anesthesia and pain management.
ABC serves several thousand anesthesiologists and CRNAs nationwide with anesthesia billing software solutions.
Please send your email address to info [at] anesthesiallc [dot] com if you would like to join the Communique mailing list!
Visit www.anesthesiallc.com for more information!
Communiqué features articles focusing on the latest hot topics for anesthesiologists, nurse anesthetists, pain management specialists and anesthesia practice administrators.
Communique is created by Anesthesia Business Consultants (ABC), the largest physician billing and practice management company specializing exclusively in the practice of anesthesia and pain management.
ABC serves several thousand anesthesiologists and CRNAs nationwide with anesthesia billing software solutions.
Please send your email address to info [at] anesthesiallc [dot] com if you would like to join the Communique mailing list!
Visit www.anesthesiallc.com for more information!
A publication dedicated to bringing articles and advice, specific to the anesthesia and pain management community, that are practical and tangible.
This edition covers the following topics:
• Using Big Data for Big Research: MPOG, NACOR and other Anesthesia Registries
• Another Year of Changes Lies Ahead for Anesthesiologists
• Disruptive Change, Anesthesiologists, and ASCs
• Performing High Acuity Cases in ASCs: The Anesthesiologist’s Role
• Endoscopy: Revisited
• Reporting Postoperative Pain Management in 2014
• 2014 CPT Coding and Key Reimbursement Changes
Phase problem sorts out all the problem which occurs after the x-ray crystallization data. In this way, we have to find out maximum values of phases and amplitude both to give the better picture of electron density map and later it is verified and validated upto maximum refined 3-D structure.
The Indian economy is classified into different sectors to simplify the analysis and understanding of economic activities. For Class 10, it's essential to grasp the sectors of the Indian economy, understand their characteristics, and recognize their importance. This guide will provide detailed notes on the Sectors of the Indian Economy Class 10, using specific long-tail keywords to enhance comprehension.
For more information, visit-www.vavaclasses.com
The Art Pastor's Guide to Sabbath | Steve ThomasonSteve Thomason
What is the purpose of the Sabbath Law in the Torah. It is interesting to compare how the context of the law shifts from Exodus to Deuteronomy. Who gets to rest, and why?
Synthetic Fiber Construction in lab .pptxPavel ( NSTU)
Synthetic fiber production is a fascinating and complex field that blends chemistry, engineering, and environmental science. By understanding these aspects, students can gain a comprehensive view of synthetic fiber production, its impact on society and the environment, and the potential for future innovations. Synthetic fibers play a crucial role in modern society, impacting various aspects of daily life, industry, and the environment. ynthetic fibers are integral to modern life, offering a range of benefits from cost-effectiveness and versatility to innovative applications and performance characteristics. While they pose environmental challenges, ongoing research and development aim to create more sustainable and eco-friendly alternatives. Understanding the importance of synthetic fibers helps in appreciating their role in the economy, industry, and daily life, while also emphasizing the need for sustainable practices and innovation.
How to Make a Field invisible in Odoo 17Celine George
It is possible to hide or invisible some fields in odoo. Commonly using “invisible” attribute in the field definition to invisible the fields. This slide will show how to make a field invisible in odoo 17.
The Roman Empire A Historical Colossus.pdfkaushalkr1407
The Roman Empire, a vast and enduring power, stands as one of history's most remarkable civilizations, leaving an indelible imprint on the world. It emerged from the Roman Republic, transitioning into an imperial powerhouse under the leadership of Augustus Caesar in 27 BCE. This transformation marked the beginning of an era defined by unprecedented territorial expansion, architectural marvels, and profound cultural influence.
The empire's roots lie in the city of Rome, founded, according to legend, by Romulus in 753 BCE. Over centuries, Rome evolved from a small settlement to a formidable republic, characterized by a complex political system with elected officials and checks on power. However, internal strife, class conflicts, and military ambitions paved the way for the end of the Republic. Julius Caesar’s dictatorship and subsequent assassination in 44 BCE created a power vacuum, leading to a civil war. Octavian, later Augustus, emerged victorious, heralding the Roman Empire’s birth.
Under Augustus, the empire experienced the Pax Romana, a 200-year period of relative peace and stability. Augustus reformed the military, established efficient administrative systems, and initiated grand construction projects. The empire's borders expanded, encompassing territories from Britain to Egypt and from Spain to the Euphrates. Roman legions, renowned for their discipline and engineering prowess, secured and maintained these vast territories, building roads, fortifications, and cities that facilitated control and integration.
The Roman Empire’s society was hierarchical, with a rigid class system. At the top were the patricians, wealthy elites who held significant political power. Below them were the plebeians, free citizens with limited political influence, and the vast numbers of slaves who formed the backbone of the economy. The family unit was central, governed by the paterfamilias, the male head who held absolute authority.
Culturally, the Romans were eclectic, absorbing and adapting elements from the civilizations they encountered, particularly the Greeks. Roman art, literature, and philosophy reflected this synthesis, creating a rich cultural tapestry. Latin, the Roman language, became the lingua franca of the Western world, influencing numerous modern languages.
Roman architecture and engineering achievements were monumental. They perfected the arch, vault, and dome, constructing enduring structures like the Colosseum, Pantheon, and aqueducts. These engineering marvels not only showcased Roman ingenuity but also served practical purposes, from public entertainment to water supply.
Unit 8 - Information and Communication Technology (Paper I).pdfThiyagu K
This slides describes the basic concepts of ICT, basics of Email, Emerging Technology and Digital Initiatives in Education. This presentations aligns with the UGC Paper I syllabus.
Welcome to TechSoup New Member Orientation and Q&A (May 2024).pdfTechSoup
In this webinar you will learn how your organization can access TechSoup's wide variety of product discount and donation programs. From hardware to software, we'll give you a tour of the tools available to help your nonprofit with productivity, collaboration, financial management, donor tracking, security, and more.
2024.06.01 Introducing a competency framework for languag learning materials ...Sandy Millin
http://sandymillin.wordpress.com/iateflwebinar2024
Published classroom materials form the basis of syllabuses, drive teacher professional development, and have a potentially huge influence on learners, teachers and education systems. All teachers also create their own materials, whether a few sentences on a blackboard, a highly-structured fully-realised online course, or anything in between. Despite this, the knowledge and skills needed to create effective language learning materials are rarely part of teacher training, and are mostly learnt by trial and error.
Knowledge and skills frameworks, generally called competency frameworks, for ELT teachers, trainers and managers have existed for a few years now. However, until I created one for my MA dissertation, there wasn’t one drawing together what we need to know and do to be able to effectively produce language learning materials.
This webinar will introduce you to my framework, highlighting the key competencies I identified from my research. It will also show how anybody involved in language teaching (any language, not just English!), teacher training, managing schools or developing language learning materials can benefit from using the framework.
How to Split Bills in the Odoo 17 POS ModuleCeline George
Bills have a main role in point of sale procedure. It will help to track sales, handling payments and giving receipts to customers. Bill splitting also has an important role in POS. For example, If some friends come together for dinner and if they want to divide the bill then it is possible by POS bill splitting. This slide will show how to split bills in odoo 17 POS.
Palestine last event orientationfvgnh .pptxRaedMohamed3
An EFL lesson about the current events in Palestine. It is intended to be for intermediate students who wish to increase their listening skills through a short lesson in power point.
Ethnobotany and Ethnopharmacology:
Ethnobotany in herbal drug evaluation,
Impact of Ethnobotany in traditional medicine,
New development in herbals,
Bio-prospecting tools for drug discovery,
Role of Ethnopharmacology in drug evaluation,
Reverse Pharmacology.
Star Formation in Galaxies Along the Huble Sequence
1. Star Formation In Galaxies Along The Hubble
Sequence
Robert C. Kennicut, Jr.
(Annu. Rev. Astron. Astrophys. 1998. 36:189-231)
Christian Herenz
Extragalactic Science Club 2011
March 7th, 2012
3. The Author
Robert C. Kennicut, Jr.
Foto Source: http://www.flickr.com/photos/swilliams2001/4029565601/
4. Overview
Review is basically 2 Parts:
Diagnostic methods used to measure star-formation rates
(SFRs) in galaxies.
Systematics of SFRs along the Hubble Sequence.
This talk focuses on the first part, which is not merely a
summary, but
“... a self-consistent set of SFR calibrations is presented as an
aid to workers in the field.”
(from the Abstract)
5. Outline of this Talk
Historical Overview of SFR Measurements
SFR from Evolutionary Synthesis
SFR Diagnostics
1. Continuum Luminosity - Color Scaling Relation
2. UV Continuum Luminosity
3. H Recombination Lines
4. Forbidden Lines
5. FIR Continuum Emission
Summary
6. Historical Overview of SFR Measurements
Late 1960s: First quantitative SFRs from evolutionary
synthesis models (e.g. Beatrice Tinsley 1968 - Galaxy
Colors)
1970s-80s: Development of precise direct SFR calibrators.
emission-line fluxes
(near) UV continuum
IR continuum
Application to large galaxy samples. Interpretation in terms
of evolutionary properties.
1990s - present: Detection of star-forming galaxies at
high-z. Trace evolution of SFR density with look-back time
(e.g. Madau plot)
7. SFRs from Evolutionary Synthesis
Individual stars in galaxies typically unresolved
−→ SFRs derive from integrated light (Colors, UV, IR,
recombination lines).
Basis of all calibrators: Evolutionary Synthesis Models
(ESM)
Grid of stellar evolution tracks ˆ= T (t) & Lbol.
(t) for various
M .
Stellar atmosphere modells or spectral libraries: T (t) &
Lbol.
→ broadband colors or spectra (ˆ=Templates(t))
weighed by IMF Templates(t) = Luminosity, Color (and
spectrum) for single age population
For different SFH: Use linear-combination of single age
pops.
4 free parameters (at least): age, metalicity /
metal-abundance, IMF, SFH (constant / e−τ ...)
Synthesis modells can be downloaded / generated online
(e.g. GALEXV - Bruzal & Charlot)
8. SFR Diagnostic I. – Continuum Luminosity - Color
Scaling
Color dictated by ratio of early to late-type stars
Color ⇒ Fraction of young (t < 109y) massive stars
Knowledge of amount of massive stars: IMF → SFR
Scales via broad band L to total stellar mass
109
y old pop., Salpeter IMF, e−τ
SFH
9. SFRs via Continuum Luminosity - Color Scaling
Pros:
Easy applicable for homogeneous sample, when no
absolute accuracy is required.
Cons / Gotchas:
IMF dependent, age, metalicity & SFH (holds for all
calibrators)
Reddening (!)
Imprecise & prone to systematic errors
10. SFR Diagnostic II. - UV Luminosity
Direct tracer: UV (1250 ˚A – 2500 ˚A) photons produced only by
massive O – B Type Stars (no attenuation by Lyα forest & no
contribution by old stars).
Fλ of O0 (red), B8 (blue) and G5×5000 (green) type stars
11. For Salpeter IMF 0.1 . . . 100M , continuous SFH tPop = 108 yrs:
SFR[M yr−1
] = 1.4 × 10−28
Lν[erg s−1
Hz−1
] (1)
Pros:
Directly tied to photospheric emission of young-stellar
population.
Can be used for high-redshift galaxies in the optical.
Cons / Gotchas:
Not accesible from the ground for local galaxies.
Sensitive to extinction, form of IMF (large extrapolation,
since measured M > 5M )
Inappropriate e.g. for young (t ∼ 107yrs) star-burst (lower
SFR/Lν ratio, i.e. less luminos for same SFR)
12. SFR Diagnostic III. - H Recombination Lines
Direct Tracer: Only M > 10M stars (i.e. t < 2 × 107yr)
contribute signifcantly to F(λ < 912 ˚A).
200Å 2000Å 3000Å 4000Å912Å
Λ
FΛ
For Salpeter IMF 0.1 . . . 100M , continuous SFH tPop = 108 yrs:
SFR[M yr−1
] = 1.08 × 10−53
Q(H0)[s−1
] (2)
Q(H0
)ˆ= photons with λ < 912 ˚A
13. From Eq. (2), using your “favorite recombination scenario”,
line-strengths can be derived (e.g. using tables compiled in
Osterbrock’s monograph).
For example for Case B recombination with Te = 10, 000 K:
SFR[M yr−1
] = 7.9 × 10−42
L(Hα) [erg s−1
] (3)
= 8.2 × 10−53
L(Brγ) [erg s−1
] (4)
= . . .
⇒ Recombination Lines ˆ= “Ionizing Photon Counters” (under
certain assumptions).
Parenthesis: Case B Recombination
Gas region optically thick in Lyman-Lines (generally all gas regions
that contain enough gas to be observable - because of high Lyn
line-absorption cross section - because ∝ ψi| − er|ψf
- because of . . . )
14. SFRs via hydrogen recombination lines
Pros:
High sensitivity, Hα easily measureable with small
telescopes. SFR measurable in individual regions in
nearby galaxies.
Directly coupled to most massive stars.
Cons / Gotchas:
Escape of Q(H0) photons
Extinction for Hα (but e.g. not H53α in the radio)
IMF & reliability of ESM
Hα - at high-z only with JWST.
15. Forbidden Lines ([OII])
z ∼ 0.5 Hα λ6563 shifts to IR → interest in strong bluer
lines ⇒ [OII] λ3727 (doublet).
Excitation dependent on abundance and ionization state of
gas, i.e. not directly coupled to ionizing flux.
Empirical calibration to Hα Eq. 3 (using a set of ∼ 170
galaxies) yields:
SFR[M yr−1
] = (1.4 ± 0.4) × 10−41
L([OII]) [erg s−1
] (5)
Pros: bluer, stronger Cons: Less precise
16. FIR Continuum
Simplest Case: Radiation field dominated by young stars,
dust opacity high everywhere (dusty circumnuclear
starburst)
Dust: Absorbs essentially bolometric luminosity and
re-emits it as thermal emission (i.e. calorimetric SFR
measure).
Real Situation more complex - e.g. τ 1 approximation
not valid, dust needs to depleted by stars (i.e. old
generation contributes to dust heating) - etc.
Models from literature calibrated to IMF used for other
relations (±30%):
SFR[M yr−1
] = 4.5 × 10−44
LFIRo(8 − 1000µm) [erg s−1
]
(6)
10 – 100 Myr old starburst
17. Summary
Several tracers (UV, Lines, FIR) for SFR exist, but quantitative
calibration is tricky and requires a set of assumptions. Provided
that for a galaxy or sample of galaxies the assumptions given in
this review are valid, the formulas
SFR[M yr−1
] = 1.4 × 10−28
Lν[erg s−1
Hz−1
]
SFR[M yr−1
] = 7.9 × 10−42
L(Hα) [erg s−1
]
= 8.2 × 10−53
L(Brγ) [erg s−1
]
= . . .
SFR[M yr−1
] = (1.4 ± 0.4) × 10−41
L([OII]) [erg s−1
]
SFR[M yr−1
] = 4.5 × 10−44
LFIRo(8 − 1000µm) [erg s−1
]
can be used.