Galaxies 626. Lecture 10 The history of star formation from far infrared and radio observations
|
|
- Posy Berry
- 5 years ago
- Views:
Transcription
1 Galaxies 626 Lecture 10 The history of star formation from far infrared and radio observations
2 Cosmic Star Formation History Various probes of the global SF rate: ρ* (z) M yr 1 comoving Mpc 3 UV continuum (U band surveys, GALEX, LBGs) Hα and [O II] emission in spectroscopic surveys mid IR dust emission 1.4 GHz radio emission
3 Cosmic SFH: Calibration Kennicutt 1998 Ann Rev A&A 36, 189 (Salpeter IMF) UV continuum ( Å) : Pro: Extensive datasets over 0<z<6; know stellar evolutionary tracks & w/imf, # of stars in a given mass interval, so know light produced each λ Con: dust! IMF dependence 2. Line emission (Hα, [O II]) : Pro: Very sensitive probe, available to z~2 (lose in thermal IR) Con: strong IMF dependence ( 3); dust (use Balmer decrement to correct); excitation uncertainties [OII] 3. Far IR emission ( µm) : Pro: Independent method, available for obscured sources to high z: Con: uncertain source of dust heating (AGN/SF?); primarily applicable in starbursts due to detection limits at high z; bolometric FIR flux required
4
5 where light emerges depends on where the stars are relative to the clouds
6 Star Formation UV ν ν IR Dust ν IR Gas Dust V U ν Dust UV ν SN Hα ν Gas e e-ee- - Radio ν IR ν
7 log Luminosity M82 a Star Forming Galaxy Efstathiou et al. MNRAS submitted 1 Wavelength 10 / µm100
8 Sllva et al The proportion is a strong function of galaxy luminosity ULIG OPT LIG FIR spiral Elliptical
9 SFR Hα SFR infrared SFR UV Comparison of Star Formation Rate Measures Star formation rates in the radio Solar masses per year Cram et al 1999
10 For the most luminous galaxies Star formation activity dominated by short lived massive stars Their UV light absorbed by dust and re emitted in FIR At higher redshifts best observed in sub mm Surveys in FIR and sub mm required to trace obscured SFR history
11 Galaxies 626 Fluxes, luminosities and K corrections
12 Luminosity Astrophysical objects tend to emit their light energy over a range of different frequencies, ν, it is thus useful to define the Luminosity( Lν) to be the energy per unit time per unit frequency interval ΔE ergs/s Hz 1 L ν= /Δν Δt L ν dν= Lν dν ν de dt Lν dν=l
13 Luminosities Important to draw a distinction between Bolometric Luminosity LBol, Total luminosity of a galaxy, measured in ergs/s or L (or absolute magnitudes) Line Luminosity e.g. LHα, Total luminosity of an emission line, measured in ergs/s or L In band power e.g. luminosity emitted in a given wavelength interval measured in ergs/s or L (or absolute magnitudes) Luminosity (density) Luminosity per unit frequency, measured in ergs/s Hz 1, often quoted as νl measured in ergs/s
14 K Correction The emission from a galaxy is observed at a different wavelength from the one that at which it was emitted due to the cosmological redshift In general one wants to compare the emission properties of galaxies at the same (emitted) wavelength The K correction is an additional term in the flux density to luminosity relationship which accounts for this difference
15 Flux density Flux density ( fν) to be the energy per unit time per unit area per unit frequency interval Watts / metre2 / Hertz, erg/s cm 2 Hz 1 f ν dν= f Jansky: 1Jy = erg/s cm 2 Hz 1 Common to see... Flux density ( fλ) the energy per unit time per unit area per unit wavelength interval Both are often simply called flux!
16 K Correction We want to relate the observed light to the light emitted at the rest frame frequencies f= L 2 1 z 2 4 πr20 S k We can see f ν ν 0 dν 0 = we know = L 4 πd2l L ν νe dνe 4 πd2l νe = 1 z ν0 dνe = 1 z dν0 f ν ν 0 dν0 = [ ] L ν ν 0 1 z 1 z dν0 4 πd 2L
17 K Correction shift of spectrum f ν ν0 = [ Band pass ] L ν ν 0 1 z 1 z 4 πd 2L
18 Galaxies at Higher z wavelength If the same object is seen further away Observed band We see the light redshifted ν0 =νe / 1 z νe = 1 z ν0 emitted feature at a fixed λ we see light emitted from bluer parts
19 galaxies at higher z Observed Band ~ 1013 Hz Emitted band ~ 1014 Hz νe = 1 z ν0 Given rest frame frequency band is observed in a narrower band thus energy per unit frequency increases dνe = 1 z dν0
20 K Correction in magnitudes If fluxes and luminosities are expressed in magnitudes m= M 5 log Hence name: K correction DL 10 pc K z Shape of spectrum and band pass correction
21 At 850 micron, as go to higher redshifts, start sampling closer to the peak of the blackbody spectrum so maintain sensitivity; negative K correction
22 FIR galaxies at high z In Sub-mm galaxies can become easier to detect at high-z
23 Galaxies 626 Galaxy populations in the submillimeter
24
25 Deep SCUBA Imaging at 850 microns Blank & Cluster Lens Fields LH NW (39 hr exposure) Barger et al A2390 cluster (22 hr exposure) Cowie, Barger & Kneib 2002
26
27 Hughes et al. 1998
28 Submillimeter Number Counts Barger et al. 1998, 1999 Scott et al Webb et al Hughes et al Blain et al Chapman et al CBK 2002
29 Submillimeter Number Counts EBL convergent fit Typical source about 1012 solar L Cowie, Barger, & Kneib 2002
30 Determining the Redshift Distribution
31 A370 SCUBA 38 hrs 2. 5' 2. 5'
32 A370 U /, R, K / 4 '' radius error circles
33 By spectroscopically observing all possible optical counterparts in the SCUBA error circles, redshifts can be determined for at least 25% of the bright SCUBA population
34 Some reliable spectroscopic identifications have been made by targeting all nearby optical sources Soucail et al Barger et al. 1999
35 Ivison et al z=2.8
36 However, in most cases the candidate optical/nir counterparts are intrinsically faint and hence difficult to identify
37 SCUBA sources with spectroscopic ids are biased towards AGN Presence of AGN makes counterpart more optically luminous AGN spectra are easier to identify
38 Not surprisingly, SCUBA sources with AGN spectra also tend to be the ones with X ray counterparts Thus, searching for counterparts to the SCUBA sources in deep X ray data reveals the presence of AGN
39 Alternative Approach for Studying the Submillimeter Sources Radio observations are useful for pinpointing the positions of the SCUBA sources (the FIR radio correlation has been empirically determined for both star formers & radio quiet AGNs) Around 60% of submm bright (>5 mjy) sources are 20cm radio sources
40 HDF N Small circles: 20cm Bigger circles: SCUBA Rectangle: GOODS ACS Large circle: DEIMOS W. H. Wang et al. 2004
41 Spectroscopy of 20cm Selected Submm Sources redshift desert radio sensitivity limit Chapman et al. (2005) 18 Keck nights ~ 100 submm sources observed ~ 70 identified median redshift = 2.2
42 Problems
43 The submm sources that are above SCUBA s blank field detection limit of 2 mjy only contribute ~20% of the total submm background Normalized to Puget et al Fixsen et al % 50% 20% 10%
44 Only 60% of the above 20% can be detected by radio telescopes to 40 microjy at 20 cm 40 µjy ULIRG LIG
45 Thus, the spectroscopically identified radio selected submm sources only represent ~10% of the total background So, we really need to learn about the faint (<2 mjy) sources A more recent approach that may be much better is a stacking analysis: (1) measure the submm fluxes at the positions of another population (2) determine the mean flux of that population (3) find the contribution to the EBL
46 For example, we can ask how much of the submillimeter background is produced by the Chandra Deep Field North hard X ray AGN sample?
47
48 When we do the stacking analysis, we find that AGN contribute only 15% of the 850µm background Thus, most of the submm EBL is probably due to star formation
49 Typical Source about 0.7mJy Barger et al. 1998,1999 Scott et al Webb et al Hughes et al Blain et al Chapman et al CBK 2002 Need another population with at least a surface density of ~25000/deg2 to identify the EBL
50 Clear that the current 20 cm samples do not have enough sources There are only marginally enough 24 micron sources Thus, the current 20 cm and 24 micron samples are not deep enough to have reached the fainter submm sources
51 However, NIR samples are deep enough 20 x 20 shown RJK
52 Band N <S850> Iν (mjy) (Jy Deg 2) ULB 1.6 µm ± ± 2.4 IRAC 3.6 µm ± ± 3.4 MIPS 24 µm ± ± 1.1 VLA 20 cm ± ± µm µm ± 2.0 We can see that 20 cm samples are good at picking out the brighter submm sources, but there aren t enough of them to produce the EBL; NIR does best!
53 Submm EBL vs Spectral Type Sd? E Sb Intrinsically Red Irr Sc Intrinsically Blue
54 Submm EBL vs Redshift core Near IR sample
55 Contrast with the brighter sources: fainter sources peak at lower redshifts core Near IR sample Chapman et al. (2005)
56 Dusty Star Formation History Compute 20 cm EBL vs z for all the sources contributing to the submillimeter light (the core sample)
57 Dusty Star Formation History Translate into a bolometric luminosity density using the FIR radio correlation Convert to a star formation rate density [using Kennicutt 1998] A submm analysis gives the same answer at z>1 (where the sources are near ULIRGs) but is subject to assumptions about the dust temperature
58
59 Comparison of the FIR determined star formation with the UV determined star formation Maximal corrections for missing EBL, if at z=1 3 Directly measured FIR star formation ρ t
60 At low redshifts, the correction from the UV is not so large, but at higher redshifts, it is factors of 3 5 (green curves) ρ t
61 These results are similar to estimates of the extinction correction made from the UV continuum characteristics of UV selected objects However, this is a little misleading, because the samples are somewhat disjoint blue star forming galaxies contribute substantially to the UV star formation but not to the FIR star formation Thus, the extinction corrections must be higher in the galaxies that produce the bulk of the FIR light and lower in the blue star forming galaxies
62 All of the backgrounds (including 850 µm) have strong contributions from below z=1; however, the UV and 850 µm come from different galaxy populations UV 850 micron 20 cm [OII]
63 Cumulative star formation history (SFH) shows actual growth of galaxies with time Cosmic baryon density Present day stellar mass density, Cole et al. (2002)
64 Summary Multiwavelength (optical/uv, NIR, submm) observations have led to a revolution in tracking the history of star formation in the universe Most (60% 80%) of the submm EBL can be detected using the NIR population and comes from intermediate type galaxies at z ~ 1 (not the same sources that dominate the UV) We have a good understanding of the evolution of the co moving density of SF since z~3, which accounts for the observed stellar mass density at z=0. Half the stars we see today were formed by z~1.4
65 The End
Galaxies 626. Lecture 9 Metals (2) and the history of star formation from optical/uv observations
Galaxies 626 Lecture 9 Metals (2) and the history of star formation from optical/uv observations Measuring metals at high redshift Metals at 6 How can we measure the ultra high z star formation? One robust
More informationMassively Star-Forming Dusty Galaxies. Len Cowie JCMT Users Meeting
Massively Star-Forming Dusty Galaxies Len Cowie JCMT Users Meeting The luminous dusty star-formation history: We are using SCUBA-2 to address three questions What fraction of the SF is in luminous dusty
More informationLecture 10. (1) Radio star formation rates. Galaxy mass assembly history
Lecture 10 (1) Radio star formation rates (2) Galaxy mass assembly history M82 radio/fir spectrum 1202 0725 (z = 4.7) 1335 0415 (z = 4.4) Synchrotron Free free Dust Cosmic SFH: Calibration Kennicutt 1998
More informationHigh-redshift galaxies
High-redshift galaxies Houjun Mo May 4, 2004 Galaxies can now be observed to z 6 Normal galaxies with 0.2 < z < 1 The Lyman-break population at z 3 The sub-mm sources at z 3 Between 1 2, spectroscopy desert,
More informationHigh Redshift Universe
High Redshift Universe Finding high z galaxies Lyman break galaxies (LBGs) Photometric redshifts Deep fields Starburst galaxies Extremely red objects (EROs) Sub-mm galaxies Lyman α systems Finding high
More informationStar Formation Indicators
Star Formation Indicators Calzetti 2007 astro-ph/0707.0467 Brinchmann et al. 2004 MNRAS 351, 1151 SFR indicators in general! SFR indicators are defined from the X ray to the radio! All probe the MASSIVE
More informationDusty star-forming galaxies at high redshift (part 5)
Dusty star-forming galaxies at high redshift (part 5) Flow of story 4.1.1 4.1.2 4.1.3 Millimetric Spectroscopic Redshifts Millimetric Photometric Redshifts Redshift Distributions of 24 μm selected DSFG
More informationA prelude to SKA. High-resolution mapping of the ujy radio population. Ian Smail ICC, Durham University Tom Muxlow, JBCA, University of Manchester
QuickTime and a decompressor are needed to see this picture. The University of Manchester Jodrell Bank Observatory A prelude to SKA The e-merge Legacy Survey: High-resolution mapping of the ujy radio population
More informationUV/optical spectroscopy of Submilliimeter Galaxies
UV/optical spectroscopy of Submilliimeter Galaxies Scott C. Chapman (Caltech), A. Blain (Caltech), I. Smail (Durham), M. Swinbank (Durham) R. Ivison (Edinburgh) SFR_Hα = SFR_FIR SFR_Hα = 1/10 SFR_FIR Outline:
More informationSUPPLEMENTARY INFORMATION
doi:10.1038/nature11096 Spectroscopic redshifts of CDF-N X-ray sources We have taken a recent compilation 13 as our main source of spectroscopic redshifts. These redshifts are given to two decimal places,
More informationIRS Spectroscopy of z~2 Galaxies
IRS Spectroscopy of z~2 Galaxies Houck et al., ApJ, 2005 Weedman et al., ApJ, 2005 Lutz et al., ApJ, 2005 Astronomy 671 Jason Marshall Opening the IR Wavelength Regime for Discovery One of the primary
More informationDeep Surveys or How We Learn About the Early Universe When We Can t Measure All that Would Be Nice!
Deep Surveys or How We Learn About the Early Universe When We Can t Measure All that Would Be Nice! Presented at the AAS Seminar on Infrared Astronomy, AAS Meeting, Jan 7, 2003, Seattle Marcia Rieke mrieke@as.
More informationTHE GAS MASS AND STAR FORMATION RATE
THE GAS MASS AND STAR FORMATION RATE OF STAR-FORMING GALAXIES AT z ~ 1.3 Nissim Kanekar National Centre for Radio Astrophysics, Pune Apurba Bera Shiv Sethi Ben Weiner K. Dwarakanath Image: B. Premkumar
More informationThe History of Star Formation. Mark Dickinson, NOAO
The History of Star Formation Mark Dickinson, NOAO Hopkins & Beacom 2 Star formation rate vs. redshift Madau et al. 1996 Star formation rate vs. redshift Madau et al. 1996 Hopkins & Beacom 2006 Stellar
More informationMulti-wavelength Surveys for AGN & AGN Variability. Vicki Sarajedini University of Florida
Multi-wavelength Surveys for AGN & AGN Variability Vicki Sarajedini University of Florida What are Active Galactic Nuclei (AGN)? Galaxies with a source of non-stellar emission arising in the nucleus (excessive
More information9. Evolution with redshift - z > 1.5. Selection in the rest-frame UV
11-5-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c09-1 11-5-10see http://www.strw.leidenuniv.nl/ franx/college/galaxies10 10-c09-2 9. Evolution with redshift - z > 1.5 Selection in
More informationWHAT CAN WE LEARN ABOUT SUBMILLIMETER GALAXIES FROM INTERFEROMETRIC IMAGING? Joshua D. Younger Harvard/CfA
WHAT CAN WE LEARN ABOUT SUBMILLIMETER GALAXIES FROM INTERFEROMETRIC IMAGING? Joshua D. Younger Harvard/CfA J. D. Younger, G. G. Fazio, J. Huang (CfA) M. S. Yun, G. Wilson, T. Perera, K. Scott, J. Austermann
More informationResults from the Chandra Deep Field North
Results from the Chandra Deep Field North Brandt, Alexander, Bauer, Garmire, Hornschemeier, Immler, Lehmer, Schneider, Vignali, Wu, Barger, Cowie, Bautz, Nousek, Sargent, Townsley Chandra Deep Field North
More informationDistant galaxies: a future 25-m submm telescope
Distant galaxies: a future 25-m submm telescope Andrew Blain Caltech 11 th October 2003 Cornell-Caltech Workshop Contents Galaxy populations being probed Modes of investigation Continuum surveys Line surveys
More informationarxiv: v1 [astro-ph.ga] 16 Oct 2018
New Parameter Space for Deep Field Radio Continuum Surveys arxiv:1810.07143v1 [astro-ph.ga] 16 Oct 2018 Amy J. Barger, 1 Kotaro Kohno, 2 Eric J. Murphy 3, Mark T. Sargent 4, and James J. Condon 3 1 University
More informationTowards a Complete Census of Extreme Starbursts in the Early Universe
Towards a Complete Census of Extreme Starbursts in the Early Universe Caitlin M. Casey, University of Cambridge (University of Hawai i - September 2010) Scott Chapman, Ian Smail, Rob Ivison, Andrew Blain,
More informationMeasuring star formation in galaxies and its evolution. Andrew Hopkins Australian Astronomical Observatory
Measuring star formation in galaxies and its evolution Andrew Hopkins Australian Astronomical Observatory Evolution of Star Formation Evolution of Star Formation Evolution of Star Formation Evolution of
More informationX-ray emission from star-forming galaxies
X-ray emission from star-forming galaxies, Marat Gilfanov & Rashid Sunyaev (Max Planck Institute for Astrophysics) Ultra-Luminous X-ray sources and Middle Weight Black Holes Monday May 24th, 2010 - ESAC
More informationDusty star-forming galaxies at high redshift (part 5)
Dusty star-forming galaxies at high redshift (part 5) Flow of story 4.1 4.2 4.3 Acquiring Spectroscopic or Photometric Redshifts Infrared SED Fitting for DSFGs Estimating L IR, T dust and M dust from an
More informationX-raying galactic feedback in nearby disk galaxies. Q. Daniel Wang University of Massachusetts
X-raying galactic feedback in nearby disk galaxies Q. Daniel Wang University of Massachusetts Chandra survey of diffuse X-ray emission from 53 edge-on galaxies i > 60 o, D < 30 Mpc (Li, J.-T. & Wang, Q.D.
More informationLecture 11: SDSS Sources at Other Wavelengths: From X rays to radio. Astr 598: Astronomy with SDSS
Astr 598: Astronomy with SDSS Spring Quarter 4, University of Washington, Željko Ivezić Lecture : SDSS Sources at Other Wavelengths: From X rays to radio Large Surveys at Many Wavelengths SDSS: UV-IR five-band
More informationP. ANDREANI Dipartimento di Astronomia, Università di Padova, Italy MPI f. Extraterrestrische Physik, Garching, Germany
EXTREMELY RED AND DUSTY GALAXIES P. ANDREANI Dipartimento di Astronomia, Università di Padova, Italy MPI f. Extraterrestrische Physik, Garching, Germany A. CIMATTI Osservatorio Astronomico di Arcetri,
More informationThe star-formation history of mass-selected galaxies in the VIDEO survey
The star-formation history of mass-selected galaxies in the VIDEO survey Jonathan Zwart jz@uwcastro.org 18 September, 2013 OVERVIEW Measuring Star-Formation Rates (SFRs) The VISTA Deep Extragalactic Observations
More informationarxiv: v1 [astro-ph.co] 27 May 2009
**FULL TITLE** ASP Conference Series, Vol. **VOLUME**, **YEAR OF PUBLICATION** **NAMES OF EDITORS** The Pedigrees of DOGs (Dust-Obscured Galaxies) arxiv:0905.453v [astro-ph.co] 27 May 2009 Arjun Dey National
More informationSTAR FORMATION RATES observational overview. Ulrike Kuchner
STAR FORMATION RATES observational overview Ulrike Kuchner Remember, remember.. Outline! measurements of SFRs: - techniques to see what the SF rate is - importance of massive stars and HII regions - the
More informationGas Accretion & Outflows from Redshift z~1 Galaxies
Gas Accretion & Outflows from Redshift z~1 Galaxies David C. Koo Kate Rubin, Ben Weiner, Drew Phillips, Jason Prochaska, DEEP2, TKRS, & AEGIS Teams UCO/Lick Observatory, University of California, Santa
More informationALMA and the high redshift Universe. Simon Lilly ETH Zürich
Simon Lilly ETH Zürich 2012 will be an exciting year 2012 a great year ? Cool material is central to this process Galaxy formation at high z (Hauser and Dwek ARAA 2001) Extragalactic background light:
More informationThe Herschel Multi-tiered Extragalactic Survey (HerMES) The Evolution of the FIR/SMM Luminosity Function and of the Cosmic SFRD
The Herschel Multi-tiered Extragalactic Survey (HerMES) The Evolution of the FIR/SMM Luminosity Function and of the Cosmic SFRD Lucia Marchetti University of Padova - Open University Mattia Vaccari - University
More informationGALAXIES 626 Spring Introduction: What do we want to learn?
GALAXIES 626 Spring 2007 Introduction: What do we want to learn? The light of the universe is in discrete chunks: Why? How did we get from the tiny density fluctuations at recombination to the beautifully
More informationGalaxy Evolution at High Redshift: The Future Remains Obscure. Mark Dickinson (NOAO)
Galaxy Evolution at High Redshift: The Future Remains Obscure Mark Dickinson (NOAO) Galaxy Evolution at High Redshift: The Future Remains Obscure Past Mark Dickinson (NOAO) IRAS FIDEL 60μm MIPS 160μm 70μm
More informationDemographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers?
Elaine M. Sadler Black holes in massive galaxies Demographics of radio galaxies nearby and at z~0.55 Are radio galaxies signposts to black-hole mergers? Work done with Russell Cannon, Scott Croom, Helen
More informationPhotons. Observational Astronomy 2018 Part 1 Prof. S.C. Trager
Photons Observational Astronomy 2018 Part 1 Prof. S.C. Trager Wavelengths, frequencies, and energies of photons Recall that λν=c, where λ is the wavelength of a photon, ν is its frequency, and c is the
More informationRadio Afterglows. What Good are They? Dale A. Frail. National Radio Astronomy Observatory. Gamma Ray Bursts: The Brightest Explosions in the Universe
Radio Afterglows What Good are They? Dale A. Frail National Radio Astronomy Observatory Gamma Ray Bursts: The Brightest Explosions in the Universe The 2 nd Harvard-Smithsonian Conference on Theoretical
More informationA mid and far-ir view of the star formation activity in galaxy systems and their surroundings
A mid and far-ir view of the star formation activity in galaxy systems and their surroundings Andrea Biviano Andrea Biviano INAF/Osservatorio Astronomico di Trieste Outline: mid-ir & multiwavelength observations
More informationMolecular Gas and the Host Galaxies of Infrared-Excess Quasi-Stellar Objects
Molecular Gas and the Host Galaxies of Infrared-Excess Quasi-Stellar Objects A. S. Evans (Stony Brook) J. A. Surace & D. T. Frayer (Caltech) D. B. Sanders (Hawaii) Luminous Infrared Galaxies Properties
More informationStellar Populations: Resolved vs. unresolved
Outline Stellar Populations: Resolved vs. unresolved Individual stars can be analyzed Applicable for Milky Way star clusters and the most nearby galaxies Integrated spectroscopy / photometry only The most
More informationThe micro- and nano-jy sky
The micro- and nano-jy sky Paolo Padovani, ESO, Germany The sub-mjy source population Which type of sources will SKA see at micro-jy and nano-jy flux densities? How many of them and how faint? Which multi-wavelength
More informationAy 20 Basic Astronomy and the Galaxy Problem Set 2
Ay 20 Basic Astronomy and the Galaxy Problem Set 2 October 19, 2008 1 Angular resolutions of radio and other telescopes Angular resolution for a circular aperture is given by the formula, θ min = 1.22λ
More informationPaul Sell. University of Wisconsin-Madison Advisor: Christy Tremonti
A SAMPLE OF EXTREME MERGER-DRIVEN STARBURST GALAXIES AS VIEWED BY THE CHANDRA AND HUBBLE SPACE TELESCOPES Paul Sell University of Wisconsin-Madison Advisor: Christy Tremonti Collaboration: Aleks Diamond-Stanic,
More informationMulti-wavelength ISM diagnostics in high redshift galaxies
Multi-wavelength ISM diagnostics in high redshift galaxies Alexandra Pope (UMass Amherst) Transformational Science in the ALMA Era: Multi-Wavelength Studies of Galaxy Evolution Conference Charlottesville,
More informationMolecules at High Redshift (CO in Spitzer and Herschel-selected High-z Samples) David T. Frayer (NRAO), H-ATLAS, GOODS-H, FIDEL, and Zpectrometer
Molecules at High Redshift (CO in Spitzer and Herschel-selected High-z Samples) David T. Frayer (NRAO), H-ATLAS, GOODS-H, FIDEL, and Zpectrometer Teams Frayer (1) Background! IRAS ULIRG/LIRGs showed good
More information13.1 Galaxy Evolution: Introduction
13.1 Galaxy Evolution: Introduction Galaxies Must Evolve Stars evolve: they are born from ISM, evolve, shed envelopes or explode, enriching the ISM, more stars are born Structure evolves: density fluctuations
More informationMultiwavelength Study of Distant Galaxies. Toru Yamada (Subaru Telescope, NAOJ)
Multiwavelength Study of Distant Galaxies Toru Yamada (Subaru Telescope, NAOJ) Studying Galaxy Formation with ALMA 1. Studying Galaxy Forming Region with ALMA 2. Multi-wavelength Study of Galaxy Formation/Evolution
More informationMOS: A critical tool for current & future radio surveys Daniel J.B. Smith, University of Hertfordshire, UK.
MOS: A critical tool for current & future radio surveys Daniel J.B. Smith, University of Hertfordshire, UK www.herts.ac.uk/~dsmith/ MOS: A critical tool for current & future radio surveys Outline Why study
More informationGRB Host Galaxies and the Uses of GRBs in Cosmology
GRB Host Galaxies and the Uses of GRBs in Cosmology S. G. Djorgovski for the Caltech-NRAO-CARA GRB Collaboration: S.R. Kulkarni, D.A. Frail, F.A. Harrison, R. Sari, J.S. Bloom, E. Berger, P. Price, D.
More informationPOLYCYCLIC AROMATIC HYDROCARBON CONTRIBUTION TO THE INFRARED OUTPUT ENERGY OF THE UNIVERSE AT Z 2
The Astrophysical Journal Supplement Series, 154:112 117, 2004 September # 2004. The American Astronomical Society. All rights reserved. Printed in U.S.A. POLYCYCLIC AROMATIC HYDROCARBON CONTRIBUTION TO
More informationThe Cosmic History of Star Formation. James Dunlop Institute for Astronomy, University of Edinburgh
The Cosmic History of Star Formation James Dunlop Institute for Astronomy, University of Edinburgh PLAN 1. Background 2. Star-formation rate (SFR) indicators 3. The last ~11 billion years: 0 < z < 3 4.
More informationRadio Nebulae around Luminous Blue Variable Stars
Radio Nebulae around Luminous Blue Variable Stars Claudia Agliozzo 1 G. Umana 2 C. Trigilio 2 C. Buemi 2 P. Leto 2 A. Ingallinera 1 A. Noriega-Crespo 3 J. Hora 4 1 University of Catania, Italy 2 INAF-Astrophysical
More informationConcentra)on of dusty starbursts and AGNs at a z=3.09 proto- cluster core
September 9,2015 at Soverato, Italy Concentra)on of dusty starbursts and AGNs at a z=3.09 proto- cluster core Hideki Umehata (ESO, U. Tokyo) Kotaro Kohno, Yoichi Tamura (U. Tokyo), et al 1 Outlines Introduction
More informationMultiwavelength Observations of Dust-Obscured Galaxies Revealed by Gamma-Ray Bursts
Multiwavelength Observations of Dust-Obscured Galaxies Revealed by Gamma-Ray Bursts Hubble Fellow Caltech, Department of Astronomy IPAC Seminar Collaborators Brad Cenko Joshua Bloom Adam Morgan Nial Tanvir
More informationRadio Quiet AGN: Black Hole & Host Galaxy Proper;es
Radio Quiet AGN: Black Hole & Host Galaxy Proper;es (ESO) Collaborators: V. Mainieri, P. Padovani, P. Rosa6, N. Miller, K. I. Kellermann, P. Tozzi, S. Va>akunnel, A. Bongiorno, + PEP Collaboration Credit:
More informationSurvey of dusty AGNs based on the mid-infrared all-sky survey catalog
Survey of dusty AGNs based on the mid-infrared all-sky survey catalog Shinki Oyabu (Nagoya University) & MSAGN team 1. Introduction 2. MSAGN 3. Results 1. AKARI results 2. Other activity 4. Dusty AGNs
More informationALMA Science Ex am ples
ALMA Science Ex am ples Min S. Yun (UMass/ ANASAC) ALMA Science Requirements High Fidelity Imaging Precise Imaging at 0.1 Resolution Routine Sub- mjy Continuum Sensitivity Routine mk Spectral Sensitivity
More informationAstr 2320 Thurs. April 27, 2017 Today s Topics. Chapter 21: Active Galaxies and Quasars
Astr 2320 Thurs. April 27, 2017 Today s Topics Chapter 21: Active Galaxies and Quasars Emission Mechanisms Synchrotron Radiation Starburst Galaxies Active Galactic Nuclei Seyfert Galaxies BL Lac Galaxies
More informationObserving the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics
Observing the Formation of Dense Stellar Nuclei at Low and High Redshift (?) Roderik Overzier Max-Planck-Institute for Astrophysics with: Tim Heckman (JHU) GALEX Science Team (PI: Chris Martin), Lee Armus,
More informationAge Dating A SSP. Quick quiz: please write down a 3 sentence explanation of why these plots look like they do.
Color is only a weak function of age after ~3Gyrs (for a given metallicity) (See MBW pg 473) But there is a strong change in M/L V and weak change in M/L K Age Dating A SSP Quick quiz: please write down
More informationSurvey of dusty AGNs based on the mid-infrared all-sky survey catalog. Shinki Oyabu (Nagoya University) & MSAGN team
Survey of dusty AGNs based on the mid-infrared all-sky survey catalog Shinki Oyabu (Nagoya University) & MSAGN team Search for Active Galactic Nuclei Purpose 1 The MIR selection can minimize wavelength-dependent
More informationarxiv:astro-ph/ v1 18 Aug 2001
Accepted for publication in ApJL Preprint typeset using L A TEX style emulateapj v. 25/04/01 THE CONSEQUENCES OF THE COSMIC STAR-FORMATION RATE: X-RAY NUMBER COUNTS A. Ptak 1, R. Griffiths Carnegie Mellon
More informationScience with the Intermediate Layer
Science with the Intermediate Layer 20 deg 2 to depth of grizy=28.6,28.1,27.7,27.1,26.6 10 7 Mpc 3 at z 2 Jenny E. Greene (Princeton/Carnegie, Hubble Fellow) Watching Galaxies Assemble Thomas et al. 2005
More informationarxiv:astro-ph/ v2 15 May 2001
Current Star Formation in Post-Starburst Galaxies? Neal A. Miller 1 National Radio Astronomy Observatory 2, P.O. Box O, Socorro, New Mexico 87801 arxiv:astro-ph/0105151v2 15 May 2001 nmiller@aoc.nrao.edu
More informationGalaxies. Need a (physically) meaningful way of describing the relevant properties of a galaxy.
Galaxies Aim to understand the characteristics of galaxies, how they have evolved in time, and how they depend on environment (location in space), size, mass, etc. Need a (physically) meaningful way of
More informationThe Far-Infrared Radio Correlation in Galaxies at High Redshifts
The Far-Infrared Radio Correlation in Galaxies at High Redshifts Plan A My own work aims and methodology My results so far Implications of my results What I plan to do next brief summary of the FIR-Radio
More informationCosmological Background Radiation and Extragalactic Gamma-ray Opacity
Cosmological Background Radiation and Extragalactic Gamma-ray Opacity Rudy Gilmore SISSA TeV Particle Astrophysics July 21, 2010 Collaborators: Joel Primack - UCSC Rachel Somerville - STScI (Baltimore)
More informationsummary of last lecture
radiation specific intensity flux density bolometric flux summary of last lecture Js 1 m 2 Hz 1 sr 1 Js 1 m 2 Hz 1 Js 1 m 2 blackbody radiation Planck function(s) Wien s Law λ max T = 2898 µm K Js 1 m
More informationAstro2010 Science White Paper: Tracing the Mass Buildup of Supermassive Black Holes and their Host Galaxies
Astro2010 Science White Paper: Tracing the Mass Buildup of Supermassive Black Holes and their Host Galaxies Anton M. Koekemoer (STScI) Dan Batcheldor (RIT) Marc Postman (STScI) Rachel Somerville (STScI)
More informationBUILDING GALAXIES. Question 1: When and where did the stars form?
BUILDING GALAXIES The unprecedented accuracy of recent observations of the power spectrum of the cosmic microwave background leaves little doubt that the universe formed in a hot big bang, later cooling
More informationStarburst galaxies at low and high redshift
Starburst galaxies at low and high redshift Paul van der Werf Sterrewacht Leiden NAC May 28, 2004 Credits starbursts at low redshift Leonie Snijders (see poster) Frank Israel Natascha Förster Schreiber
More informationA Monster at any other Epoch:
A Monster at any other Epoch: Are Intermediate Redshift ULIRGs the Progenitors of QSO Host Galaxies? Barry Rothberg Large Binocular Telescope Observatory/George Mason University Co-Is: J. Fischer (NRL),
More informationActive Galactic Nuclei SEDs as a function of type and luminosity
Active Galactic Nuclei SEDs as a function of type and luminosity Mari Polletta (IASF-INAF Milan) Collaborators: L. Chiappetti (IASF-INAF), L. Maraschi, M. Giorgetti, G. Trinchieri (Brera-INAF), B. Wilkes
More informationUltra Luminous Infared Galaxies. Yanling Wu Feb 22 nd,2005
Ultra Luminous Infared Galaxies Yanling Wu Feb 22 nd,2005 The Biggest and the brightest Biggest and the best & best and the brightest Definition: LIRG: L8-1000umL
More informationTHE XMM-NEWTON AND SPITZER VIEW OF GALAXY/AGN FORMATION AT. F.J. Carrera, J. Ebrero 1, M.J. Page 2, and J.A. Stevens 3
1 THE XMM-NEWTON AND SPITZER VIEW OF GALAXY/AGN FORMATION AT F.J. Carrera, J. Ebrero 1, M.J. Page 2, and J.A. Stevens 3 1 Instituto de Física de Cantabria, Avenida de los Castros, 39005 Santander, Spain
More informationDusty star-forming galaxies at high redshift (part 7)
Dusty star-forming galaxies at high redshift (part 7) Flow of story 4 Redshifts and Spectral Energy Distributions of Infrared- Luminous Galaxies 5 Physical Characterization 1 Physical Characterization
More informationDark Matter. ASTR 333/433 Spring Today Stars & Gas. essentials about stuff we can see. First Homework on-line Due Feb. 4
Dark Matter ASTR 333/433 Spring 2016 Today Stars & Gas essentials about stuff we can see First Homework on-line Due Feb. 4 Galaxies are made of stars - D. Silva (1990) private communication Stars Majority
More informationLyα-Emitting Galaxies at z=3.1: L* Progenitors Experiencing Rapid Star Formation
Lyα-Emitting Galaxies at z=3.1: L* Progenitors Experiencing Rapid Star Formation Gawiser et al., 2007 Presented on October 22, 2009 PHYS 689: Galaxy Formation Lyman-α Emitters (LAEs) Lyα line is easily
More informationQuasars and AGN. What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs
Goals: Quasars and AGN What are quasars and how do they differ from galaxies? What powers AGN s. Jets and outflows from QSOs and AGNs Discovery of Quasars Radio Observations of the Sky Reber (an amateur
More informationThe evolution of the Galaxy Stellar Mass Function:
The evolution of the Galaxy Stellar Mass Function: towards the high-mass end at high redshifts Helena Domínguez Sánchez Jordi Cepa (IAC), Miguel Sánchez Portal (ESAC), Andrea Cimatti (UniBo), Francesca
More informationSTAR FORMATION ALONG A CLUSTER-FEEDING FILAMENT
STAR FORMATION ALONG A CLUSTER-FEEDING FILAMENT DARIO FADDA IPAC / Caltech Outline * Discovery of the filament * The obscured star formation in different environments * Radio observation and the density
More informationRevealing new optically-emitting extragalactic Supernova Remnants
10 th Hellenic Astronomical Conference Ioannina, September 2011 Revealing new optically-emitting extragalactic Supernova Remnants Ioanna Leonidaki (NOA) Collaborators: P. Boumis (NOA), A. Zezas (UOC, CfA)
More informationActive Galactic Nuclei OIII
Active Galactic Nuclei In 1908, Edward Fath (1880-1959) observed NGC 1068 with his spectroscope, which displayed odd (and very strong) emission lines. In 1926 Hubble recorded emission lines of this and
More informationStar-formation Across Cosmic Time: Initial Results from the e-merge Study of the μjy Radio Source Population. SPARCs VII The Precursors Awaken
Star-formation Across Cosmic Time: Initial Results from the e-merge Study of the μjy Radio Source Population SPARCs VII The Precursors Awaken Tom Muxlow & Nick Wrigley JBCA Manchester for the e-merge Consortium
More informationEVLA + ALMA represent > 10x improvement in observational capabilities from 1GHz to 1 THz
What is EVLA? Build on existing infrastructure, replace all electronics (correlator, Rx, IF, M/C) => multiply ten-fold the VLA s observational capabilities 80x Bandwidth (8 GHz, full stokes), with 4000
More informationThe ALMA z=4 Survey (AR4S)
The ALMA z=4 Survey (AR4S) ALMA studies of massive z~4-5 galaxies Corentin Schreiber Leiden University October 21 2016 In collaboration with: Maurilio Pannella, David Elbaz, Roger Leiton, Tao Wang, and
More informationDominik A. Riechers Cornell University
JVLA ALMA CCAT First year of full science Finishing construction The next big thing The Interstellar Medium in High Redshift Galaxies Dominik A. Riechers Cornell University Phases of the ISM MPIA Summer
More informationRadio Properties Of X-Ray Selected AGN
Radio Properties Of X-Ray Selected AGN Manuela Molina In collaboration with: M. Polletta, L. Chiappetti, L. Paioro (INAF/IASF-Mi), G.Trinchieri (OA Brera), F. Owen (NRAO) and Chandra/SWIRE Team. Astrosiesta,
More informationChapter 10: Unresolved Stellar Populations
Chapter 10: Unresolved Stellar Populations We now consider the case when individual stars are not resolved. So we need to use photometric and spectroscopic observations of integrated magnitudes, colors
More informationDust properties of galaxies at redshift z 5-6
Dust properties of galaxies at redshift z 5-6 Ivana Barisic 1, Supervisor: Dr. Peter L. Capak 2, and Co-supervisor: Dr. Andreas Faisst 2 1 Physics Department, University of Zagreb, Zagreb, Croatia 2 Infrared
More informationSupernova and Star Formation Rates
Supernova and Star Formation Rates Enrico Cappellaro Istituto Nazionale di Astrofisica Osservatorio Astronomico di Padova SN vs. SF rates Kennicutt 1998 SFR vs. galaxy color from evolutionary synthesis
More informationThe Contribution of Active Galactic Nuclei to the Excess Cosmic Radio Background at 1.4 GHz
The Contribution of Active Galactic Nuclei to the Excess Cosmic Radio Background at 1.4 GHz David R. Ballantyne Center for Relativistic Astrophysics, School of Physics, Georgia Tech The Cosmic Backgrounds
More informationFar-infrared Herschel SPIRE spectroscopy reveals physical conditions of ionised gas in high-redshift lensed starbursts
Far-infrared Herschel SPIRE spectroscopy reveals physical conditions of ionised gas in high-redshift lensed starbursts Zhi-Yu (Z-Y) Zhang 张智昱 U. Edinburgh/ESO Outline Background Sample description Herschel
More informationX ray Survey Results on AGN Physics and Evolution Niel Brandt
X ray Survey Results on AGN Physics and Evolution Niel Brandt Chandra XMM Newton Photon statistics Hard response ACIS Best positions Highest sens. < 6 kev 50 250 times sens. of previous missions Good positions
More informationExtended Chandra Multi-Wavelength Project (ChaMPx): Source Catalog and Applications
Extended Chandra Multi-Wavelength Project (ChaMPx): Source Catalog and Applications Dong-Woo Kim, P. Green, T. L. Aldcroft, W. Barkhouse, D. Haggard, V. Kashyap, A. Mossman, M. A. Agueros, A. Constantin,
More informationQuasars ASTR 2120 Sarazin. Quintuple Gravitational Lens Quasar
Quasars ASTR 2120 Sarazin Quintuple Gravitational Lens Quasar Quasars Quasar = Quasi-stellar (radio) source Optical: faint, blue, star-like objects Radio: point radio sources, faint blue star-like optical
More informationAstronomy 330 Lecture Dec 2010
Astronomy 330 Lecture 26 10 Dec 2010 Outline Clusters Evolution of cluster populations The state of HI sensitivity Large Scale Structure Cluster Evolution Why might we expect it? What does density determine?
More informationRest-frame Optical Spectra: A Window into Galaxy Formation at z~2
Rest-frame Optical Spectra: A Window into Galaxy Formation at z~2 Alice Shapley (UCLA) Collaborators: Mariska Kriek, Naveen Reddy, Brian Siana, Alison Coil, Bahram Mobasher, Bill Freeman, Ryan Sanders,
More informationHow to measure star formation rates in galaxies?
How to measure star formation rates in galaxies? Véronique Buat 1 1. Aix-Marseille Université, CNRS, LAM (Laboratoire d Astrophysique de Marseille) UMR7326, 13388, Marseille, France Our knowledge of cosmic
More information