Probing the reioniza.on epoch with ALMA

Size: px
Start display at page:

Download "Probing the reioniza.on epoch with ALMA"

Transcription

1 Probing the reioniza.on epoch with ALMA Laura Pentericci INAF - Osservatorio Astronomico di Roma in collaboration with S. Carniani, A. Fontana, M. Castellano, et al. Physical characteris.cs of Normal Galaxies at z>2 Lorentz Center Workshop 19/10/2016

2 Why do we want to observe [CII]with ALMA? It is the strongest cooling line of the Interstellar medium (ISM) up to 1% of total FIR luminosity is emined in this line. It is not subject to neutral hydrogen absorp.on thus detectable in the reioniza.on epoch when Lyαα emission is increasingly suppressed for the majority of galaxies (LP +2014,2011,Schenker+2012,Ono+2012 etc ) It is a direct tracer of SFR (De Looze+2014, Sargsyan +2014) and not effected by dust as UV emission and Lyα ( but depends on metallicity ) It probes the systemic redshiz of the galaxies (important to determine ou\lows, modeling Lyα shape etc) Probes dynamical mass of the galaxy

3 Up to redshiz [CII] is detected in many LAEs and LBGs and the [CII]- SFR rela.on seems consistent with the low redshiz one (Capak +2015, WilloN+2015, Knudsen+2016) Early ALMA & PdBI searches at z> 6.5 lead to non- detec>ons Ouchi et al 2013 Himiko z=6.6 (LAE) Ota et al IOK- 1 z=6.96 (LAE) Kanekaer et al 2014 HCM6A z= (LAE) Maiolino et al BDF3299/BDF521/SDF45 (LBGs) Schaerer et al A1703- zd1/a1703- zd1 (LBGs) Gonzalez Lopez SDF LAEs Knudsen MS0451- H z=6.7 (LAE) Watson A1689- zd1 no [CII] but con.nuum detec.on Inoue SXDF- NB (LAE) [OIII] detec.on but no [CII] Also a deep non- detec.on is obtained from stacking all z 7 sources (cf Ouchi - discussion)

4 Previous ALMA observa.ons at z 7 focussed on LAEs or LBGs with strong Lyα emission Our sample à we selected bright (in UV) galaxies but with weaker Lyα emission. This was possible thanks to CANDELSz7 an ESO Large program with FORS2@VLT that allowed us to confirm the redshiz of high- z galaxies with Lyα EW as low as 3Å 7 galaxies at z>6.5 Only 4 observed during Cycle 3 EW/Å

5 Previous ALMA observa.ons at z 7 focussed on LAEs or LBGs with strong Lyα emission Our sample à we selected bright (in UV) galaxies but with weaker Lyα emission. This was possible thanks to CANDELSz7 an ESO Large program with FORS2@VLT that allowed us to confirm the redshiz of high- z galaxies with Lyα EW as low as 3Å 7 galaxies at z>6.5 Only 4 observed during Cycle 3 EW/Å

6 We obtain detec.ons for all 4 observed targets with S/N >4.5 *The detec.ons are marginally resolved. *We observed significant spa.al offset (>0.1 ) in 2 cases. *NTTDF6563 was observed on two separate runs (Cycle 2&3) and confirmed on both sets None of the galaxy is detected In the con.nuum SFR dust = L IR [L ] 6-7 M yr - 1 à SFR TOT SFR UV

7 Spa.al offsets are observed in many other cases: do we have an issue with ALMA astrometry or is this a physical effect? our 4 galaxies From lez to right: BDF3299@z=7.109 (Maiolino+2015), (Knudsen+2016), RXJ1347:1216@z=6.765(Bradac+2016) Some of the z 5.5 galaxies in Capak+2015 Cumula.ve distribu.on of radial separa.on between 16 ALMA sources and their HST near- IR counter- parts. Blue line is azer shizing the HST frame (Dunlop+2016)

8 Velocity offset Contrary to the Lyα emission line, the [CII] traces the systemic redshiz of the galaxies à We can measure the ΔV=z Lyα z systemic Values are 100 km/s à quite small for objects with MUV = compared to lower redshiz galaxies of similar brightness

9 Velocity offset vs M UV Compila.on of Δv Lyα at various redshizs z=7 LP+2016,[CII], Inoue+2015 [OIII], Sobral+2016 [HeII], Stark+2015 CIII] Maiolino+2015[CII], Bradac+2016[CII] For a given M UV the z 7 galaxies tend to have lower ΔV=z Lyα z systemic although the sta.s.cs is limited especially for faint sources z=6 Willot+2015,Knudsen+2016 [CII] z=3.8 Schenker+2013 z=3 LBGs and LAEs Erb+2014 z=3 deep stacks of VUDS sources Guaita+in prep. z=2 LAEs and LBGs Erb+2014

10 Offset vs Lyα EW Offset vs redshiz z=7 bright objects

11 Possible origin of smaller offset In shell models (Verhamme+2015,Gronke+2015) this is related to smaller neutral hydrogen gas column densi.es (N HI <10 20 cm - 2) and to reduced ou\low veloci.es Gallerani+2016 find evidence for ou\lowing gas gas with v out =180 km/s at z 5.5 by stacking the[cii] spectra by Capack+2015 and modelling the broad wing residuals (not yet doable with z 7 data) In many recent models connec.ng Lyα to LyC proper.es, small velocity offsets (of the Lyα line compared to systemic) are one indica.on of possible LyC leakers (Dijkstra+2016, Verhamme +2015). In galaxies with low neutral hydrogen column density and/or low covering factor there are some special routes that facilitate the escape of both Lyα and ionizing photons

12 A consequence of the smaller offsets (either for lower ou\lows or column densi.es) is that less neutral hydrogen in the IGM would be needed to explain the drop in the visibility of Lyα emission from z 6 to z 7 N H The fraction of Lyα photons, f trans, transmitted through a fully neutral IGM at z=10, as a function of outflowing velocity v sh for N H i = cm 2 (red) and N H i =10 21 cm 2 (blue). Outflows of 50 km s 1 boost f trans (Dijkstra+2009) Comparison between observed Lyα EW distribu.on at z=7 and model predic.ons assuming v=200 km/s implies ΔΧ HI 0.51 (LP+2014)

13 The SFR- [CII] rela.on: do we see a [CII] deficit (or not)? Our galaxies(+bradac) are a factor of 3 less luminous in [CII] compared to local and z 5.5 galaxies with similar SFR. Is this (combined with the many undetec.ons) a solid indica.on of [CII] deficit? Some points to consider 1)SFR is the total of uncorrected UV + dust obscured SFR. Some objects could be shizing along the x- axis 2) Galaxies compactness: should we use surface brightness instead of [CII] luminosi.es? (cf Herrera- Camus+2015) 3) [CII] could be broader than ini.ally predicted - - early es.mates on limits where done using a width of 40-50km/s (e.g. Gonzalez- Lopez +2014, Ota+2014). Our highest S/N line has FWHM=250km/s 4)Metallicity effect

14 Supposing the deficit is confirmed what causes it? Model by Vallini+2015 (improved version of Vallini+2013) Emission from cold and warm neutral medium + PDR regions Constant distribu.on of metallicity in the gas/ metallicity scales with density Very high spa.al resolu.on (60 pc) Includes increased effect of CMB on the [CII] Lines Emission from PDR regions dominate Possible explana.ons of the observed [CII] deficit are 1) Nega.ve stellar feedback: the molecular clouds in the central parts of primordial galaxies (sites of strong star forma.on) are rapidly disrupted by stellar feedback. As a result [CII] emission arises only from more external accre.ng/satellite clumps of neutral gas. This effect can explain the spa.ally offset emission in some galaxies between the center of SF and that of CII emission. 2) Low gas metallicity 3) A combina.on of the above

15 Simulation of a primeval galaxy at z = 7.1 with SFR similar to BDF3299. (a) The distribution of column density of ionized gas (which emits Lyα) is shown in colours The black points show the distribution of young stars (UV continuum, which dominates the Y-band emission in our images). The contours show the emission of [C ii] tracing the neutral gas (distributed in clumps orbiting/accreting the primary galaxy). (b) Same as the top panel but the ionized gas has been convolved with the angular resolution of ground based images (0.5 arcsec) and the [C ii] map has been convolved with the ALMA beam of our data. a b (c) Integrated [C ii] spectrum from the whole simulation. c Maiolini+2015, Vallini+2015

16 Do we see a trend in terms of galaxy proper.es? Lyα eminers have limits that point to lower [CII] emission The 3 red dashed lines are models from Vallini+2015 with different metallici.es (0.2 Z /0.1 Z 0.05Z ) Blue points: low Lyα EW à Z 0.1 Z (including the new Bradac+2016 lensed galaxy) Green points intermediate EW à Z<0.1 Z Red points: high Lyα EW> 50 Å à Z<0.05Z Lyα eminers are believed to have lower metallicity compared to the general LBG popula.on LAEs at z 2.5 have average 0.2 Z with some of the faintest being consistent with Z (Trainor+2016) (see also Erb+2014,Erb+2016 Also consistent with the recent detec.on of [OIII]88μm in the LAESXDF- NB1006-2, at z=7.215 and with high Lya EW (>75 Å). This galaxy shows no [CII] emission implying high [OIII]/[CII] ra.o (Inoue+2016). Such high ra.os are observed in local metal poor dwarf galaxies (Cormier+2015)

17 Can we use [CII] efficiently to determine the redshiz when the Lyα line is not present e.g. during the reioniza.on epoch for the large majority of galaxies? From CANDELSz7 we have selected the 9 brightest confirmed i- drop (z= ) (DeBarros+in prep) with visible con.nuum + Lyman break (or very weak Lyα) such that the redshiz is constrained to bener than Approved for Cycle 4 observa.ons For these galaxies we don t need spectral scanning since the redshiz is already reasonably well constrained by our ultra- deep spectra.

18 New ALMA observa.ons of the [OIII]88μm emission is detected with S/N=5.5 spa.al and 6.5 spectral 0.3 The [OIII] line is offset both spa.ally (0.3 compared to near- IR emission) and in velocity (+400 Km/s compared to Lyα) The [OIII] and [CII] emission are offset compared to the HST image but also not co- spa>al between them. In the inset the emission from a bright nearby serendipitous source showing the good alignment between the [CII] and [OIII] maps à the offset is real (Carniani et al. in prepara.on)

Unveiling the nature of z 6 galaxies through [CII] emission studies

Unveiling the nature of z 6 galaxies through [CII] emission studies Unveiling the nature of z 6 galaxies through [CII] emission studies Simona Gallerani in collabora=on with: Livia Vallini, Andrea Ferrara, Andrea PalloMni, Roberto Maiolino, Chiara Feruglio, Dominik Riechers,

More information

Investigating the connection between LyC and Lyα emission and other indirect indicators

Investigating the connection between LyC and Lyα emission and other indirect indicators Investigating the connection between LyC and Lyα emission and other indirect indicators F. Marchi, L. Pentericci, L. Guaita, D. Schaerer, M. Castellano, B. Ribeiro and the VUDS collaboration Emission line

More information

Unveiling the nature of bright z ~ 7 galaxies with HST and JWST

Unveiling the nature of bright z ~ 7 galaxies with HST and JWST Unveiling the nature of bright z ~ 7 galaxies with HST and JWST Rebecca Bowler Hintze Fellow, University of Oxford Nicholas Kurti Junior Fellow, Brasenose College with Jim Dunlop, Ross McLure, Derek McLeod,

More information

Wagg ea. [CII] in ALMA SV 20min, 16 ants. 334GHz. SMA 20hrs

Wagg ea. [CII] in ALMA SV 20min, 16 ants. 334GHz. SMA 20hrs BRI1202-0725 z=4.7 HyLIRG (10 13 L o ) pair SFR ~ few 10 3 M o yr -1 4 + SMG + Salome ea. CO 5-4 + M H2 ~ 10 11 M o QSO + HST 814 Hu ea 96 SMA [CII] 158um 334GHz, 20hrs Iono ea 2007 [CII] in 1202-0725

More information

arxiv: v1 [astro-ph.ga] 31 Aug 2016

arxiv: v1 [astro-ph.ga] 31 Aug 2016 DRAFT VERSION SEPTEMBER 1, 2016 Preprint typeset using LATEX style emulateapj v. 5/2/11 TRACING THE REIONIZATION EPOCH WITH ALMA: [CII] EMISSION IN Z 7 GALAXIES L. PENTERICCI 1, S.CARNIANI 2,3, M. CASTELLANO

More information

Alaina Henry Goddard Space Flight Center

Alaina Henry Goddard Space Flight Center Lyman α emission from Green Peas The Role of Circumgalactic Gas Density, Covering, and Kinematics Alaina Henry Goddard Space Flight Center Imaged Lyα from a Green Pea galaxy Hayes et al. (2014) Claudia

More information

Primeval Starbursting Galaxies: Presentation of Lyman-Break Galaxies by Mauro Giavalisco. Jean P. Walker Rutgers University

Primeval Starbursting Galaxies: Presentation of Lyman-Break Galaxies by Mauro Giavalisco. Jean P. Walker Rutgers University Primeval Starbursting Galaxies: Presentation of Lyman-Break Galaxies by Mauro Giavalisco Jean P. Walker Rutgers University Outline Context within Galaxy Forma>on History of Primeval Galaxies Deconstruct

More information

Emission lines in star-forming galaxies

Emission lines in star-forming galaxies Emission lines in star-forming galaxies Daniel Schaerer (Geneva Observatory & CNRS) Introduction Properties of CIII] and CIV emitters at high redshift Compact strong emission line galaxies at z~0.3: analogs

More information

On the Detectability of Lyman Alpha Emission by Galaxies from the Epoch of Reionization. Mark Dijkstra (MPA, Garching)

On the Detectability of Lyman Alpha Emission by Galaxies from the Epoch of Reionization. Mark Dijkstra (MPA, Garching) On the Detectability of Lyman Alpha Emission by Galaxies from the Epoch of Reionization Mark Dijkstra (MPA, Garching) Outline Why we care about the HI Lya line. Lya transfer basics. Why direct detection

More information

High-Redshift Galaxies: A brief summary

High-Redshift Galaxies: A brief summary High-Redshift Galaxies: A brief summary Brant Robertson (Caltech) on behalf of David Law (UCLA), Bahram Mobasher (UCR), and Brian Siana (Caltech/Incoming CGE) Observable Cosmological History t~3.7x10 5

More information

Lyα Galaxies as a Probe of the High-z Universe. Mark Dijkstra

Lyα Galaxies as a Probe of the High-z Universe. Mark Dijkstra Lyα Galaxies as a Probe of the High-z Universe Mark Dijkstra Credit: Andrew Chung (MPA) Credit: Max Gronke (Oslo) The Suppressed Lyα flux from galaxies at z>6 `Lyα fraction Stark et al., Pentericci et

More information

Lya as a Probe of the (High-z) Universe

Lya as a Probe of the (High-z) Universe Lya as a Probe of the (High-z) Universe Mark Dijkstra (CfA) Main Collaborators: Adam Lidz, Avi Loeb (CfA) Stuart Wyithe (Melbourne), Zoltan Haiman (Columbia) Lya as a Probe of the (High-z) Universe Outline

More information

The First Galaxies: Evolution drivers via luminosity functions and spectroscopy through a magnifying GLASS

The First Galaxies: Evolution drivers via luminosity functions and spectroscopy through a magnifying GLASS Charlotte Mason (UCLA) Aspen, 7 Feb 2016 The First Galaxies: Evolution drivers via luminosity functions and spectroscopy through a magnifying GLASS with Tommaso Treu (UCLA), Michele Trenti (U. Melbourne),

More information

The evolution of bright galaxies at z > 6

The evolution of bright galaxies at z > 6 The evolution of bright galaxies at z > 6 the power of degree-scale, near-infrared surveys Rebecca Bowler Hintze Fellow, University of Oxford with Jim Dunlop, Ross McLure, Matt Jarvis, Derek McLeod, H.

More information

Fine-structure line diagnostics of the SFR and ISM conditions

Fine-structure line diagnostics of the SFR and ISM conditions Fine-structure line diagnostics of the SFR and ISM conditions Ilse De Looze 1, Diane Cormier 2,3, Suzanne Madden 2, Sacha Hony 3, Vianney Lebouteiller 2, Eric Pellegrini 3, with inputs of the Dwarf Galaxy

More information

Seeing Through the Trough: Detecting Lyman Alpha from Early Generations of Galaxies

Seeing Through the Trough: Detecting Lyman Alpha from Early Generations of Galaxies Seeing Through the Trough: Detecting Lyman Alpha from Early Generations of Galaxies Mark Dijkstra (ITC) collaborators: Stuart Wyithe, Avi Loeb, Adam Lidz, Zoltan Haiman Schematic History of the Universe

More information

Remarkable Disk and Off Nuclear Starburst Ac8vity in the Tadpole Galaxy as Revealed by the Spitzer Space Telescope

Remarkable Disk and Off Nuclear Starburst Ac8vity in the Tadpole Galaxy as Revealed by the Spitzer Space Telescope Remarkable Disk and Off Nuclear Starburst Ac8vity in the Tadpole Galaxy as Revealed by the Spitzer Space Telescope T.H. JarreE, M. PolleEa, I.P Fournon et al. Presenta8on by: William Gray Date: 2/27/09

More information

High-Redshift Galaxies at the Epoch of Cosmic Reionization

High-Redshift Galaxies at the Epoch of Cosmic Reionization High-Redshift Galaxies at the Epoch of Cosmic Reionization Linhua Jiang ( 江林华 ) (KIAA, Peking University) 2014 KIAA-PKU Astrophysics Forum Collaborators: F. Bian, B. Clement, S. Cohen, R. Dave, E. Egami,

More information

Emission lines from galaxies in the Epoch of Reioniza5on

Emission lines from galaxies in the Epoch of Reioniza5on Emission lines from galaxies in the Epoch of Reioniza5on Simona Gallerani Emanuele Sobacchi, Andrea Ferrara, Livia Vallini, Andrea PalloBni, CarloDa Gruppioni, Andrei Mesinger Monte Mario, Roma, SPICA

More information

Outline: Part II. The end of the dark ages. Structure formation. Merging cold dark matter halos. First stars z t Univ Myr.

Outline: Part II. The end of the dark ages. Structure formation. Merging cold dark matter halos. First stars z t Univ Myr. Outline: Part I Outline: Part II The end of the dark ages Dark ages First stars z 20 30 t Univ 100 200 Myr First galaxies z 10 15 t Univ 300 500 Myr Current observational limit: HST and 8 10 m telescopes

More information

Masami Ouchi (University of Tokyo)

Masami Ouchi (University of Tokyo) Pushing the Redshi- Fron1er towards the First- Star Forma1on Epoch with Subaru 2010 (830: 5hr) 2011 (600: 4hr) 2011 (830: 2hr) z Lya =7.213 z Lya =7.308 MO et al. in prep. Ono, MO et al. (2011) Masami

More information

Galaxies 626. Lecture 5

Galaxies 626. Lecture 5 Galaxies 626 Lecture 5 Galaxies 626 The epoch of reionization After Reionization After reionization, star formation was never the same: the first massive stars produce dust, which catalyzes H2 formation

More information

The formation of super-stellar clusters

The formation of super-stellar clusters The formation of super-stellar clusters François Boulanger Institut d Astrophysique Spatiale Cynthia Herrera, Edith Falgarone, Pierre Guillard, Nicole Nesvadba, Guillaume Pineau des Forets Outline How

More information

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 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 information

arxiv: v1 [astro-ph.ga] 1 Jun 2018

arxiv: v1 [astro-ph.ga] 1 Jun 2018 Publ. Astron. Soc. Japan (214) (), 1 22 doi: 1.193/pasj/xxx 1 arxiv:186.486v1 [astro-ph.ga] 1 Jun 218 Big Three Dragons : a z =7.15 Lyman Break Galaxy Detected in [OIII] 88 µm, [CII] 158 µm, and Dust Continuum

More information

Simulating high-redshift galaxies

Simulating high-redshift galaxies Simulating high-redshift galaxies Pratika Dayal Collaborators : Andrea Ferrara, Stefano Borgani, Alex Saro, Luca Tornatore, Stefania Salvadori, Hiroyuki Hirashita, Simona Gallerani, Antonella Maselli,

More information

Gas Masses and Gas Fractions: Applications of the Kennicutt- Schmidt Law at High Redshift

Gas Masses and Gas Fractions: Applications of the Kennicutt- Schmidt Law at High Redshift Gas Masses and Gas Fractions: Applications of the Kennicutt- Schmidt Law at High Redshift Dawn Erb (CfA) Kennicutt-Schmidt Workshop, UCSD December 19, 2006 Overview Properties of star-forming galaxies

More information

arxiv: v1 [astro-ph.ga] 16 Aug 2017

arxiv: v1 [astro-ph.ga] 16 Aug 2017 Draft version September 4, 2018 Typeset using LATEX twocolumn style in AASTeX61 SÍGAME SIMULATIONS OF THE [C II], [O I] AND [O III] LINE EMISSION FROM STAR FORMING GALAXIES AT Z 6 Karen Olsen, 1 Thomas

More information

The The largest assembly ESO high-redshift. Lidia Tasca & VUDS collaboration

The The largest assembly ESO high-redshift. Lidia Tasca & VUDS collaboration The The largest assembly ESO high-redshift of massive Large galaxies Programme at 2

More information

[CII] intensity mapping with CONCERTO

[CII] intensity mapping with CONCERTO Aspen Intensity Mapping Conference, 4-9 Feb 2018 [CII] intensity mapping with CONCERTO Matthieu Béthermin on behalf of the CONCERTO team PI: Lagache (thanks for providing slides); Instrument scientist:

More information

Stellar Populations: Resolved vs. unresolved

Stellar 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 information

Understanding Lyα Emission Using LBGs (and vice versa)

Understanding Lyα Emission Using LBGs (and vice versa) Understanding Lyα Emission Using LBGs (and vice versa) Alice Shapley (UCLA) Collaborators: Kathy Kornei, Kristin Kulas, Juna Kollmeier, Dawn Erb, Anna Quider, Max Pettini, Chuck Steidel z>1.5 Galaxy Identification

More information

The First Galaxies. Erik Zackrisson. Department of Astronomy Stockholm University

The First Galaxies. Erik Zackrisson. Department of Astronomy Stockholm University The First Galaxies Erik Zackrisson Department of Astronomy Stockholm University Outline The first galaxies what, when, why? What s so special about them? Why are they important for cosmology? How can we

More information

Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010

Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010 Payne-Scott workshop on Hyper Compact HII regions Sydney, September 8, 2010 Aim Review the characteristics of regions of ionized gas within young massive star forming regions. Will focus the discussion

More information

V2'#$0D*:$0()%"*,-.!/ K'(B5*2#*0D; T2&3B5U

V2'#$0D*:$0()%*,-.!/ K'(B5*2#*0D; T2&3B5U V2'#$0D*:$0()%"*,-.!/ K'(B5*2#*0D; T2&3B5U 2 S-Cam NB101 Observations KONNO ET AL. tion. The previous studies suggest that the fraction of strong LAEs in Lyman break galaxies (LBGs) decreases from z 6

More information

Shedding light on hyperluminous quasars at the golden epoch of AGN/galaxy coevolu<on

Shedding light on hyperluminous quasars at the golden epoch of AGN/galaxy coevolu<on Shedding light on hyperluminous quasars at the golden epoch of AGN/galaxy coevolu

More information

SOFIA/GREAT observations of LMC-N 11: Does [C ii] trace regions with a large H 2 fraction?

SOFIA/GREAT observations of LMC-N 11: Does [C ii] trace regions with a large H 2 fraction? SOFIA/GREAT observations of LMC-N 11: Does [C ii] trace regions with a large H 2 fraction? Vianney Lebouteiller Laboratoire AIM - CEA, Saclay, France Main collaborators: F. Galliano, S. Madden, M. Chevance,

More information

DLAs Probing Quasar Host Galaxies. Hayley Finley P. Petitjean, P. Noterdaeme, I. Pâris + SDSS III BOSS Collaboration 2013 A&A

DLAs Probing Quasar Host Galaxies. Hayley Finley P. Petitjean, P. Noterdaeme, I. Pâris + SDSS III BOSS Collaboration 2013 A&A DLAs Probing Quasar Host Galaxies Hayley Finley P. Petitjean, P. Noterdaeme, I. Pâris + SDSS III BOSS Collaboration 2013 A&A 558 111 Outline Feedback mechanisms in QSO host galaxies Strong DLAs at zqso

More information

EUCLID Legacy with Spectroscopy

EUCLID Legacy with Spectroscopy EUCLID Legacy with Spectroscopy Gianni Zamorani INAF - Bologna Astronomical Observatory (on behalf of the E-NIS Team) Observing the Dark Universe with Euclid 17-18 November 2009 ESTEC, The Netherlands

More information

HST & Resolved Stellar Popula3ons

HST & Resolved Stellar Popula3ons HST & Resolved Stellar Popula3ons Resolved stellar popula3ons provides a powerful tool to follow galaxy evolu3on consistently and directly in terms of physical parameters such as age (star forma3on history),

More information

Star Formation Indicators

Star 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 information

Observations and Inferences from Lyman-α Emitters

Observations and Inferences from Lyman-α Emitters Observations and Inferences from Lyman-α Emitters Christopher J. White 6 March 2013 Outline 1 What Are Lyα Emitters? 2 How Are They Observed? 3 Results and Inferences 4 HSC 5 Conclusion The Lyα Line n

More information

Introduction and Motivation

Introduction and Motivation 1 Introduction and Motivation This last two days at this conference, we ve focused on two large questions regarding the role that AGNs play in galaxy evolution: My research focuses on exploring these questions

More information

Measuring the evolution of the star formation rate efficiency of neutral atomic hydrogen gas from z ~1 4

Measuring the evolution of the star formation rate efficiency of neutral atomic hydrogen gas from z ~1 4 Measuring the evolution of the star formation rate efficiency of neutral atomic hydrogen gas from z ~1 4 Marc Rafelski Galactic Scale Star Formation August 2012 Collaborators: Harry Teplitz Arthur Wolfe

More information

High Redshift Universe

High 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 information

The parsec scale of. ac-ve galac-c nuclei. Mar Mezcua. International Max Planck Research School for Astronomy and Astrophysics

The parsec scale of. ac-ve galac-c nuclei. Mar Mezcua. International Max Planck Research School for Astronomy and Astrophysics The parsec scale of ESO ac-ve galac-c nuclei International Max Planck Research School for Astronomy and Astrophysics COST Ac(on MP0905 - Black Holes in a Violent Universe In collaboration with A. Prieto,

More information

Neon Emission in HST Emission- Line Galaxies at z 2. Greg Zeimann

Neon Emission in HST Emission- Line Galaxies at z 2. Greg Zeimann Neon Emission in HST Emission- Line Galaxies at z 2 Greg Zeimann grzeimann@psu.edu Using radia@ve transfer modeling to infer the physical condi@ons of the warm ionized gas and the ionizing source Modeling

More information

Dust properties of galaxies at redshift z 5-6

Dust 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 information

Test #1! Test #2! Test #2: Results!

Test #1! Test #2! Test #2: Results! High-Redshift Galaxies II - Populations (cont d) - Current Redshift Frontier - Gravitational Lensing I will hand back Test #2 HW#10 will be due next Monday. Nov 18, 2015 Test #1 Test #2 Test #2: Results

More information

UV/optical spectroscopy of Submilliimeter Galaxies

UV/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 information

Search for the FIRST GALAXIES

Search for the FIRST GALAXIES Search for the FIRST GALAXIES R. Pelló IRAP - Institut de Recherche en Astrophysique et Planétologie 1 XIème Ecole de Cosmologie : 17-22 Sep 2012 (Cargèse) Outline 1. Looking for the first galaxies a)

More information

Jens Melinder. With financial support from CNES/CNRS convention #

Jens Melinder. With financial support from CNES/CNRS convention # Jens Melinder With financial support from CNES/CNRS convention # 131425 u u u u The Lyman-α line in emission u The hydrogen Lyman-α emission line is the intrinsically brightest spectral feature from star-forming

More information

Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of ngvla Working Group 2

Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of ngvla Working Group 2 Next Generation Very Large Array Working Group 2 HI in M74: Walter+ 08 CO in M51: Schinnerer+ 13 Continuum in M82: Marvil & Owen Galaxy Ecosystems Adam Leroy (OSU), Eric Murphy (NRAO/IPAC) on behalf of

More information

Spectral Energy Distribution of galaxies

Spectral Energy Distribution of galaxies Spectral Energy Distribution of galaxies Paola Santini PhD in Astronomy, Astrophysics and Space Science A.A. 2013 2014 Key points lecture 1 Multiwavalength astronomy: 1. Gives a complete view of the galaxy

More information

arxiv: v2 [astro-ph.ga] 2 Sep 2018

arxiv: v2 [astro-ph.ga] 2 Sep 2018 Astronomy & Astrophysics manuscript no. cola1_xsh c ESO 2018 September 5, 2018 Confirmation of double peaked Lyα emission at z = 6.593 Witnessing a galaxy directly contributing to the reionisation of the

More information

Gas Accretion & Outflows from Redshift z~1 Galaxies

Gas 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 information

Star-forming galaxies at high-z with the JWST!

Star-forming galaxies at high-z with the JWST! Star-forming galaxies at high-z with the JWST Daniel Schaerer (Geneva Observatory, CNRS) Motivation + open question Physical properties of high-z star-forming galaxies need for direct emission line measurements

More information

ALMA Synergy with ATHENA

ALMA Synergy with ATHENA ALMA Synergy with ATHENA Françoise Combes Observatoire de Paris 9 September 2015 ALMA & Athena: common issues Galaxy formation and evolution, clustering Surveys of galaxies at high and intermediate redshifts

More information

Physical conditions of the interstellar medium in star-forming galaxies at z~1.5

Physical conditions of the interstellar medium in star-forming galaxies at z~1.5 Physical conditions of the interstellar medium in star-forming galaxies at z~1.5 Abstract Masao Hayashi (NAOJ, Mitaka) Subaru seminar @ Subaru Telescope, NAOJ 10 March 2015 To be re-submitted soon to PASJ

More information

Gasflows in Galaxy Clusters

Gasflows in Galaxy Clusters Gasflows in Galaxy Clusters Brian McNamara University of Waterloo Perimeter Ins7tute for Theore7cal Physics, Canada H. Russell, C.J. Ma, A. Vantyghem, C. Kirkpatrick, R. Main P. Nulsen, A. Edge, A., Fabian,

More information

Astronomy II (ASTR-1020) Homework 2

Astronomy II (ASTR-1020) Homework 2 Astronomy II (ASTR-1020) Homework 2 Due: 10 February 2009 The answers of this multiple choice homework are to be indicated on a Scantron sheet (either Form # 822 N-E or Ref # ABF-882) which you are to

More information

Unraveling the distribution of ionized gas in the Galactic plane with radio recombination lines.

Unraveling the distribution of ionized gas in the Galactic plane with radio recombination lines. Unraveling the distribution of ionized gas in the Galactic plane with radio recombination lines. Jorge Pineda, Shinji Horiuchi, Tom Kuiper, Geoff Bryden, Melissa Soriano, and Joe Lazio Jet Propulsion Laboratory

More information

Probing the End of Dark Ages with High-redshift Quasars. Xiaohui Fan University of Arizona Dec 14, 2004

Probing the End of Dark Ages with High-redshift Quasars. Xiaohui Fan University of Arizona Dec 14, 2004 Probing the End of Dark Ages with High-redshift Quasars Xiaohui Fan University of Arizona Dec 14, 2004 High-redshift Quasars and the End of Cosmic Dark Ages Existence of SBHs at the end of Dark Ages BH

More information

Multiwavelength Study of Distant Galaxies. Toru Yamada (Subaru Telescope, NAOJ)

Multiwavelength 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 information

Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines!

Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines! Some HI is in reasonably well defined clouds. Motions inside the cloud, and motion of the cloud will broaden and shift the observed lines Idealized 21cm spectra Example observed 21cm spectra HI densities

More information

Emission Lyα dans les galaxies starburst

Emission Lyα dans les galaxies starburst Emission Lyα dans les galaxies starburst D. Kunth, D. Schaerer; M. Hayes; G. Ostlin, J.M. Mas-Hesse; A. Verhamme; C. Leitherer; A. Petrosian Institut d'astrophysique de Paris Atelier MUSE Lyon, 7- Lyα

More information

Herschel Virgo Cluster Survey (HeViCS) Jonathan Davies for the HeViCS consortium

Herschel Virgo Cluster Survey (HeViCS) Jonathan Davies for the HeViCS consortium Herschel Virgo Cluster Survey (HeViCS) Jonathan Davies for the HeViCS consortium ESO, Garching, June 2011 HeViCS Consor&um Members Davies, J. I.; Baes, M.; Bendo, G. J.; Bianchi, S.; Bomans, D. J.; Boselli,

More information

Molecular clouds (see review in astro-ph/990382) (also CO [12.1,12.2])

Molecular clouds (see review in astro-ph/990382) (also CO [12.1,12.2]) Molecular clouds (see review in astro-ph/990382) (also CO [12.1,12.2]) Massive interstellar gas clouds Up to ~10 5 M 100 s of LY in diameter. Giant Molecular Clouds (GMCs) defined to be M > 10 4 M High

More information

Chris Pearson: RAL Space. Chris Pearson: April

Chris Pearson: RAL Space. Chris Pearson: April Chris Pearson: RAL Space 1 2 Young Star Dust Clouds Infra Red Light 3 Starlight reprocessed to infrared wavelengths 4 1983: The Dawn of Infrared Astronomy Infra-Red Astronomical Satellite (IRAS) All sky

More information

ASTRO 310: Galac/c & Extragalac/c Astronomy Prof. Jeff Kenney. Class 7 Sept 19, 2018 The Milky Way Galaxy: Gas: HII Regions

ASTRO 310: Galac/c & Extragalac/c Astronomy Prof. Jeff Kenney. Class 7 Sept 19, 2018 The Milky Way Galaxy: Gas: HII Regions ASTRO 310: Galac/c & Extragalac/c Astronomy Prof. Jeff Kenney Class 7 Sept 19, 2018 The Milky Way Galaxy: Gas: HII Regions importance of HII regions one of main ISM phases great example for understanding

More information

High-Redshift Galaxies - Exploring Galaxy Evolution - Populations - Current Redshift Frontier

High-Redshift Galaxies - Exploring Galaxy Evolution - Populations - Current Redshift Frontier Lecture 20; Nov 06, 2017 High-Redshift Galaxies - Exploring Galaxy Evolution - Populations - Current Redshift Frontier Pick up PE #20 Reading: Chapter 9 of textbook I will hand back HW#7 Wednesday: Second

More information

The skin of Orion. Molecular Astrophysics: The Herschel and ALMA era PRESS RELEASE

The skin of Orion. Molecular Astrophysics: The Herschel and ALMA era PRESS RELEASE Molecular Astrophysics: The Herschel and ALMA era PRESS RELEASE The skin of Orion 9- October- 2015 Imaging Orion in ionized carbon emission. Among the brightest emissions from the interstellar medium and

More information

The dust mass in z > 6 normal star-forming galaxies

The dust mass in z > 6 normal star-forming galaxies MNRAS 451, L70 L74 (2015) doi:10.1093/mnrasl/slv070 The dust mass in z > 6 normal star-forming galaxies Mattia Mancini, 1,2 Raffaella Schneider, 1 Luca Graziani, 1 Rosa Valiante, 1 Pratika Dayal, 3 Umberto

More information

Concentra)on of dusty starbursts and AGNs at a z=3.09 proto- cluster core

Concentra)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 information

A prelude to SKA. High-resolution mapping of the ujy radio population. Ian Smail ICC, Durham University Tom Muxlow, JBCA, University of Manchester

A 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 information

Gas 1: Molecular clouds

Gas 1: Molecular clouds Gas 1: Molecular clouds > 4000 known with masses ~ 10 3 to 10 5 M T ~ 10 to 25 K (cold!); number density n > 10 9 gas particles m 3 Emission bands in IR, mm, radio regions from molecules comprising H,

More information

Protostellar Jets in the ngvla Era

Protostellar Jets in the ngvla Era Protostellar Jets in the ngvla Era Luis F. Rodríguez (IRyA- UNAM, Mexico) In collabora@on with G. Anglada, C. Carrasco- González, L. Zapata, A. Palau, R. Galván- Madrid, C. Rodríguez- Kamenetzky, A. Araudo,

More information

Astrophysics of Gaseous Nebulae

Astrophysics of Gaseous Nebulae Astrophysics of Gaseous Nebulae Astrophysics of Gaseous Nebulae Bright Nebulae of M33 Ken Crawford (Rancho Del Sol Observatory) Potsdam University Dr. Lidia Oskinova lida@astro.physik.uni-potsdam.de HST

More information

A Local Clue to the Reionization of the Universe

A Local Clue to the Reionization of the Universe A Local Clue to the Reionization of the Universe arxiv:1410.3511v1 [astro-ph.ga] 13 Oct 2014 Sanchayeeta Borthakur, 1 Timothy M. Heckman, 1 Claus Leitherer, 2 Roderik A. Overzier 3 1 Center for Astrophysical

More information

High-z QSO (HSC #123)

High-z QSO (HSC #123) Jan. 6 th, 2016 HSC/AGN meeting Next DL = 21 April High-z QSO follow-up @mm/submm (HSC #123) - especially z > 6 objects - Takuma Izumi@IoA/UTokyo takumaizumi@ioa.s.u-tokyo.ac.jp This is a submm follow-up

More information

The EMPIRE survey: CO(1-0) emission across nearby disks. Diane Cormier. Marie-Curie Fellow, AIM/CEA Saclay

The EMPIRE survey: CO(1-0) emission across nearby disks. Diane Cormier. Marie-Curie Fellow, AIM/CEA Saclay The EMPIRE survey: 13 CO(1-0) emission across nearby disks Diane Cormier Marie-Curie Fellow, AIM/CEA Saclay María-Jesús Jiménez-Donaire, Frank Bigiel (U. Heidelberg) Adam Leroy, Molly Gallagher (Ohio State),

More information

Astr 2310 Thurs. March 23, 2017 Today s Topics

Astr 2310 Thurs. March 23, 2017 Today s Topics Astr 2310 Thurs. March 23, 2017 Today s Topics Chapter 16: The Interstellar Medium and Star Formation Interstellar Dust and Dark Nebulae Interstellar Dust Dark Nebulae Interstellar Reddening Interstellar

More information

9. Evolution with redshift - z > 1.5. Selection in the rest-frame UV

9. 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 information

Interferometric Observations of S140-IRS1

Interferometric Observations of S140-IRS1 Interferometric Observations of S140-IRS1 e-merlin early science workshop April 2014 Luke T. Maud University of Leeds, UK Melvin G. Hoare University of Leeds Star formation scenario Collapse of a core

More information

The ALMA z=4 Survey (AR4S)

The 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 information

M. Dijkstra (UiO) Aspen, Mark Dijkstra. with: Shiv Sethi (RRI), Abraham Loeb (CfA), Max Gronke (UiO) & David Sobral (Lancaster)

M. Dijkstra (UiO) Aspen, Mark Dijkstra. with: Shiv Sethi (RRI), Abraham Loeb (CfA), Max Gronke (UiO) & David Sobral (Lancaster) Mark Dijkstra with: Shiv Sethi (RRI), Abraham Loeb (CfA), Max Gronke (UiO) & David Sobral (Lancaster) arxiv:1601.04712 (ApJ accepted), Dijkstra, Sethi & Loeb arxiv:1602.07695 (resubmitted to ApJ), Dijkstra,

More information

Outflows in local ULIRGS: [CII] 158 Broad Components and OH outflows

Outflows in local ULIRGS: [CII] 158 Broad Components and OH outflows Outflows in local ULIRGS: [CII] 158 Broad Components and OH outflows Natalie Christopher, University of Oxford Dr Verma and Professor Roche, University of Oxford And the SHINING team, Lead by E. Sturm,

More information

PROBING THE AGN/GALAXY CO-EVOLUTION AT ITS EXTREME

PROBING THE AGN/GALAXY CO-EVOLUTION AT ITS EXTREME THE MOST LUMINOUS QUASARS: PROBING THE AGN/GALAXY CO-EVOLUTION AT ITS EXTREME Enrico Piconcelli Osservatorio Astronomico di Roma - INAF! A. Bongiorno, F. Fiore, M. Bischetti, L. Zappacosta OA-Roma! C.

More information

Far-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 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 information

WFMOS Studies of Galaxy Formation and Reionization. Masami Ouchi (Carnegie)

WFMOS Studies of Galaxy Formation and Reionization. Masami Ouchi (Carnegie) WFMOS Studies of Galaxy Formation and Reionization Masami Ouchi (Carnegie) Outline Introduction HyperSuprime-Cam (HSC) surveys Science drivers+possible plans of WFMOS spectroscopy in the HSC survey fields

More information

Atomic Physics and the Kramers-Heisenberg Formula for Ly Alpha. Hee-Won Lee Department of Physics and Astrnomy Sejong University January 24, 2019

Atomic Physics and the Kramers-Heisenberg Formula for Ly Alpha. Hee-Won Lee Department of Physics and Astrnomy Sejong University January 24, 2019 Atomic Physics and the Kramers-Heisenberg Formula for Ly Alpha Hee-Won Lee Department of Physics and Astrnomy Sejong University January 24, 2019 Contents 1. Introduction Quasar Absorption Systems and Cosmic

More information

Paul Sell. University of Wisconsin-Madison Advisor: Christy Tremonti

Paul 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 information

The 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 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 information

Dominik A. Riechers Cornell University

Dominik 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 information

arxiv: v2 [astro-ph.ga] 17 Nov 2014

arxiv: v2 [astro-ph.ga] 17 Nov 2014 Astronomy & Astrophysics manuscript no. cii_v5_arxiv c ESO 2018 August 27, 2018 Very extended cold gas, star formation and outflows in the halo of a bright QSO at z > 6 C. Cicone 1, 2, R. Maiolino 1, 2,

More information

What do we need to know about galaxy formation?

What do we need to know about galaxy formation? What do we need to know about galaxy formation? rachel somerville University of Michigan Hubble Science Legacy Workshop April 2002 what s next? test the CDM paradigm constrain the nature of the dark matter

More information

FIR line emission from high redshift galaxies

FIR line emission from high redshift galaxies Mon. Not. R. Astron. Soc. 000, 1 6 (2012) Printed 13 May 2013 (MN LATEX style file v2.2) FIR line emission from high redshift galaxies Livia Vallini 1, Simona Gallerani 1, Andrea Ferrara 1 & Sunghye Baek

More information

Energy Sources of the Far IR Emission of M33

Energy Sources of the Far IR Emission of M33 Energy Sources of the Far IR Emission of M33 Hinz, Reike et al., ApJ 154: S259 265 (2004). Presented by James Ledoux 24 µm 70 µm 160 µm Slide 1 M33 Properties Distance 840kpc = 2.7 Mlyr (1'' ~ 4 pc) Also

More information

The Epoch of Reionization: Observational & Theoretical Topics

The Epoch of Reionization: Observational & Theoretical Topics The Epoch of Reionization: Observational & Theoretical Topics Lecture 1 Lecture 2 Lecture 3 Lecture 4 Current constraints on Reionization Physics of the 21cm probe EoR radio experiments Expected Scientific

More information

Ken-ichi Tadaki (NAOJ, JSPS research fellow)

Ken-ichi Tadaki (NAOJ, JSPS research fellow) Subaru GLAO Science Workshop June 13-14, 2013 Clumpy galaxies and compact star-forming galaxies giant clumps, compact SFGs ~ 1kpc Ken-ichi Tadaki (NAOJ, JSPS research fellow) Tadayuki Kodama (NAOJ), Ichi

More information