Multi-wavelength ISM diagnostics in high redshift galaxies

Transcription

1 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, VA August 5, 2014 Large Millimeter Telescope

2 Dust-obscured activity dominates the build-up of stars and black holes in galaxies Using data from Bouwens+2009 and Murphy+2011

3 Dust-obscured activity dominates the build-up of stars and black holes in galaxies Star formation : black BH accretion : blue, green, red Madau & Dickinson 2014

4 More molecular gas available during the peak epoch of dusty star formation and black hole growth (Mmol) [Msun Mpc -3 ] (Mstar) (HI) Keres et al. (2003) BzK Sargent et al. (2013) Obreschkow & Rawlings (2009a,b) Lagos et al. (2011) BX/BM LBG redshift z Carilli & Walter 2013

5 How do we probe the interstellar medium (gas and dust) in high redshift galaxies? Luminosity density (WHz -1 ) MIPS IRS IRAC HST Herschel SCUBA LMT ALMA VLA Circa 2014: Well sampled spectral energy distribution (SED) for high redshift Ultra Luminous Infrared Galaxies (ULIRGs, SFR ~100 M sun /yr) Rest Wavelength (µm)

6 How do we probe the interstellar medium (gas and dust) in high redshift galaxies? Luminosity density (WHz -1 ) MIPS IRS IRAC HST Herschel SCUBA LMT ALMA VLA Spitzer mid-ir spectroscopy is sensitive to the radiation heating the dust : SF or AGN Herschel imaging samples the peak of the dust emission: dust temperatures Millimeter spectroscopy (e.g. ALMA, LMT) probes the molecular gas reservoir Rest Wavelength (µm)

7 o o o Large Millimeter Telescope (LMT) 50m millimeter telescope in Mexico 15,000 ft: Excellent mm site Owned by UMass and Mexico o o Currently operating in Early Science mode as a 32.5m telescope Early science instrumentation: - AzTEC 1.1mm camera - 3mm Redshift Search Receiver (RSR) o 50 m LMT [~2016] = 1/3 the collecting area of ALMA +19 deg. latitude Time lapse video from June 2013, courtesy of James Lowenthal

8 Luminosity density (WHz -1 ) How can we probe the interstellar medium (gas and dust) in high redshift galaxies? MIPS Herschel SCUBA Rest Wavelength (µm) Spitzer mid-ir spectroscopy is sensitive to the radiation heating the dust : SF or AGN LMT Herschel imaging samples Goal: Understand IRS how dusty star formation the peak of the and dust black emission: dust temperatures hole growth proceeds during VLA the peak epoch IRAC Millimeter spectroscopy (e.g. ALMA, LMT) probes the ALMA Approach: HST Link multi-wavelength diagnostics molecular gas reservoir of the ISM in high redshift dusty galaxies

9 Session: Star Formation and Assembly of Galaxies! How is the S-K law law affected by different measurement limitations or conversion factors (from tracer molecules or emission / absorption lines to amounts of gas and SFR)?! Are the measurements from different tracers of ISM and SF consistent?! How do galaxies grow (evolve) over cosmic time?

10 Tracers of the ISM and star formation Molecular cloud PAH H 2 CO Hollenbach & Tielens 1997

11 Decomposing Spitzer mid-ir spectra into two main components: 1. Star formation: Polycyclic aromatic hydrocarbons (PAH) emission lines + extinction 2. Active Galactic Nuclei: Power-law + extinction

12 SED fitting with Spitzer/IRS + Herschel AGN dominated (mid-ir) SF dominated (mid-ir) Warm dust (~60K) Warm dust (~100K) Cool dust (~30K) Cool dust (~30K) Kirkpatrick, Pope, et al. 2012

13 SED fitting with Spitzer/IRS + Herschel AGN dominated (mid-ir) L IR,cold /L IR,total = SFR = ( ) * 1.5e-10 * L IR,total Warm dust (~100K) How does this Cool affect dust (~30K) the Schmidt-Kennicutt relation? Kirkpatrick, Pope, et al. 2012

14 Linking molecular gas and star formation at high redshift: Integrated Schmidt-Kennicutt relation Carilli & Walter 2013 Daddi et al. 2010; see also Genzel et al. 2010

15 Sample: Intermediate redshift AGN and SF galaxies log ssfr (Gyr -1 ) Star Forming Galaxy Composite AGN Main Sequence Starburst z CO 0. 5MUSES survey - z~0.2 - Spitzer/IRS spectra + Herschel imaging = decompose IR SED into SF and AGN components => SFR(L IR,SF ) - From SSFR: 14 Main Sequence 10 Starbursts Kirkpatrick, Pope, et al., 2014, ApJ submitted

16 Observations: New LMT/RSR CO(1-0) data for AGN and SF galaxies Kirkpatrick, Pope, et al., 2014, ApJ submitted

17 AGN-corrected integrated S-K relation / L CO Star Forming Galaxy Composite AGN Main Sequence Starburst Starbursts log L IR SF 1.5 SFGs f AGN,IR Fraction Kirkpatrick, Pope, et al., 2014, ApJ submitted

18 Polycyclic Aromatic Hydrocarbon (PAH) emission as a tracer of star formation Molecular cloud PAH H 2 CO Hollenbach & Tielens 1997

19 Enhanced PAH emission at high redshift L PAH,6.2 /L IR MUSES IR galaxies (z~0.08) Local ULIRGs (z~0.07) 24µm-selected (z=1-3) 70µm-selected (z~1) BzKs (z~1.5) SMGs (z~2) L IR (L O ) 10 Pope et al. 2013

20 Enhanced PAH emission at high redshift... similar to enhanced [CII] emission? L PAH,6.2 /L IR Graciá-Carpio et al MUSES IR galaxies (z~0.08) Local ULIRGs (z~0.07) 24µm-selected (z=1-3) 70µm-selected (z~1) BzKs (z~1.5) SMGs (z~2) L IR (L O ) Pope et al. 2013

21 Enhanced PAH emission at high redshift... similar to enhanced [CII] emission? L PAH,6.2 /L IR Graciá-Carpio et al MUSES IR galaxies (z~0.08) Local ULIRGs (z~0.07) 24µm-selected (z=1-3) 70µm-selected (z~1) BzKs (z~1.5) SMGs (z~2) L IR (L O ) Pope et al. 2013

22 Link between enhanced PAH emission at high redshift and more molecular gas L PAH,6.2 /L IR MUSES IR galaxies (z~0.08) Local ULIRGs (z~0.07) 24µm-selected (z=1-3) 70µm-selected (z~1) BzKs (z~1.5) SMGs (z~2) L IR (L O ) L IR /L CO(1-0) [L O / (K km s -1 pc 2 )] Pope et al. 2013

23 Link between enhanced PAH emission at high redshift and more molecular gas L PAH,6.2 /L IR MUSES IR galaxies (z~0.08) Local ULIRGs (z~0.07) 24µm-selected (z=1-3) 70µm-selected (z~1) BzKs (z~1.5) SMGs (z~2) L IR (L O ) L IR /L CO(1-0) [L O / (K km s -1 pc 2 )] Pope et al. 2013; Kirkpatrick, Pope, et al., 2014, ApJ submitted

24 Link between enhanced PAH emission at high redshift and more molecular gas L PAH,6.2 /L IR Pope et al MUSES IR galaxies (z~0.08) Local ULIRGs (z~0.07) 24µm-selected (z=1-3) 70µm-selected (z~1) BzKs (z~1.5) SMGs (z~2) L IR (L O ) L IR /L CO(1-0) [L O / (K km s -1 pc 2 )] Add [CII] to the mix ALMA! Hollenbach & Tielens 1997

25 Session: Star Formation and Assembly of Galaxies! How is the S-K law law affected by different measurement limitations or conversion factors (from tracer molecules or emission / absorption lines to amounts of gas and SFR)?! Are the measurements from different tracers of ISM and SF consistent?! How do galaxies grow (evolve) over cosmic time?

26 Session: Star Formation and Assembly of Galaxies! How is the S-K law law affected by different measurement limitations or conversion factors (from tracer molecules or emission / absorption lines to amounts of gas and SFR)? Many LIRGs/ULIRGs show concurrent black hole growth (50-80% of L IR ). Decompose IR SED to get the only the L IR,SF heated by SF. LMT pilot study: o Reduces the scatter in S-K o Brings more galaxies down onto the normal galaxy sequence

27 Session: Star Formation and Assembly of Galaxies! Are the measurements from different tracers of ISM and SF consistent? How do galaxies grow (evolve) over cosmic time? o Strong PAH emission is much more prevalent at high redshift compared to locally o Enhanced PAH emission is linked to the increased molecular gas in high redshift galaxies o Future: add links to [CII] and other ISM tracers using ALMA

28 EARLY SCIENCE WITH THE LARGE MILLIMETER TELESCOPE: EXPLORING THE EFFECT OF AGN ACTIVITY ON THE RELATIONSHIPS BETWEEN MOLECULAR GAS, DUST, AND STAR FORMATION Allison Kirkpatrick 1,AlexandraPope 1,ItziarAretxaga 2,LeeArmus 3,DanielaCalzetti 1,GeorgeHelou 4, Alfredo Montaña 2,GopalNarayanan 1,F.PeterSchloerb 1,YongShi 5,OlgaVega 2,MinYun 1 Submitted to ApJ July 12, 2014 Draft version July 12, 2014 Synergy between ALMA and LMT 50 m LMT [~2016] = 1/3 the collecting area of ALMA Wide field mm mapping Wide bandwidth CO redshift surveys