Multi-wavelength ISM diagnostics in high redshift galaxies - - PowerPoint PPT Presentation

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Multi-wavelength ISM diagnostics in high redshift galaxies - - PowerPoint PPT Presentation

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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

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Alexandra Pope (UMass Amherst) Transformational Science in the ALMA Era: Multi-Wavelength Studies of Galaxy Evolution Conference Charlottesville, VA – August 5, 2014

Multi-wavelength ISM diagnostics in high redshift galaxies

Large Millimeter Telescope

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Using data from Bouwens+2009 and Murphy+2011

Dust-obscured activity dominates the build-up of stars and black holes in galaxies

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Madau & Dickinson 2014

Dust-obscured activity dominates the build-up of stars and nd b bla lack ho k hole les in galaxies

Star formation : black BH accretion : blue, green, red

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Carilli & Walter 2013

More molecular gas available during the peak epoch of dusty star formation and black hole growth

1 2 3 5 7 107 108 109 (Mmol) [Msun Mpc-3]

(Mstar) (HI) Keres et al. (2003)

Sargent et al. (2013) Obreschkow & Rawlings (2009a,b) Lagos et al. (2011)

BzK BX/BM

  • 4

6 redshift z

LBG

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Circa 2014: Well sampled spectral energy distribution (SED) for high redshift Ultra Luminous Infrared Galaxies (ULIRGs, SFR ≥ ~100 Msun/yr) Rest Wavelength (µm) Luminosity density (WHz-1) HST VLA SCUBA MIPS IRAC Herschel IRS LMT ALMA

How do we probe the interstellar medium (gas and dust) in high redshift galaxies?

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  • 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) Luminosity density (WHz-1) HST VLA SCUBA MIPS IRAC Herschel IRS LMT ALMA

How do we probe the interstellar medium (gas and dust) in high redshift galaxies?

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Large Millimeter Telescope (LMT)

  • 50m millimeter

telescope in Mexico

  • 15,000 ft: Excellent

mm site

  • Owned by UMass

and Mexico

  • Currently operating

in Early Science mode as a 32.5m telescope

  • Early science

instrumentation:

  • AzTEC 1.1mm camera
  • 3mm Redshift Search

Receiver (RSR)

  • 50 m LMT [~2016]

= 1/3 the collecting area of ALMA

Time lapse video from June 2013, courtesy of James Lowenthal

+19 deg. latitude

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  • 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) Luminosity density (WHz-1) HST VLA SCUBA MIPS IRAC Herschel IRS LMT ALMA

How can we probe the interstellar medium (gas and dust) in high redshift galaxies?

Goal: Understand how dusty star formation and black hole growth proceeds during the peak epoch Approach: Link multi-wavelength diagnostics of the ISM in high redshift dusty galaxies

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! 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?

Session: Star F Forma mation a n and nd A Assemb mbly o ly of Ga Gala laxies

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Tracers of the ISM and star formation

Hollenbach & Tielens 1997

PAH H2 CO Molecular cloud

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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

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SED fitting with Spitzer/IRS + Herschel

AGN dominated (mid-IR) SF dominated (mid-IR)

Warm dust (~100K) Cool dust (~30K) Warm dust (~60K) Cool dust (~30K)

Kirkpatrick, Pope, et al. 2012

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SED fitting with Spitzer/IRS + Herschel

AGN dominated (mid-IR)

Warm dust (~100K) Cool dust (~30K)

LIR,cold/LIR,total = 0.2-0.5 SFR = (0.2-0.5) * 1.5e-10 * LIR,total

Kirkpatrick, Pope, et al. 2012

How does this affect the Schmidt-Kennicutt relation?

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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

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Sample: Intermediate redshift AGN and SF galaxies

Kirkpatrick, Pope, et al., 2014, ApJ submitted

0.0 0.1 0.2 0.3 zCO

  • 2.0
  • 1.5
  • 1.0
  • 0.5

0.0 0.5 1.0 log sSFR (Gyr-1)

Star Forming Galaxy Composite AGN Main Sequence Starburst Star Forming Galaxy Composite AGN Main Sequence Starburst

0.0 Fraction

5MUSES survey

  • z~0.2
  • Spitzer/IRS spectra +

Herschel imaging = decompose IR SED into SF and AGN components => SFR(LIR,SF)

  • From SSFR:

14 Main Sequence 10 Starbursts

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Observations: New LMT/RSR CO(1-0) data for AGN and SF galaxies

Kirkpatrick, Pope, et al., 2014, ApJ submitted

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“AGN-corrected” integrated S-K relation

Kirkpatrick, Pope, et al., 2014, ApJ submitted

0.0 0.1 0.2 0.3 0.4 0.5 fAGN,IR 1.0 1.5 2.0 2.5 log LIR

SF / L CO

Starbursts SFGs

Star Forming Galaxy Composite AGN Main Sequence Starburst Star Forming Galaxy Composite AGN Main Sequence Starburst

0.0 0.2 Fraction

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Polycyclic Aromatic Hydrocarbon (PAH) emission as a tracer of star formation

Hollenbach & Tielens 1997

PAH H2 CO Molecular cloud

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Enhanced PAH emission at high redshift

Pope et al. 2013

1010 1011 1012 1013 LIR (LO

  • )

0.001 0.010 LPAH,6.2/LIR

SMGs (z~2) BzKs (z~1.5) 70µm-selected (z~1) 24µm-selected (z=1-3) Local ULIRGs (z~0.07) 5MUSES IR galaxies (z~0.08)

10

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Graciá-Carpio et al. 2011

Enhanced PAH emission at high redshift ... similar to enhanced [CII] emission?

Pope et al. 2013 1010 1011 1012 1013 LIR (LO

  • )

0.001 0.010 LPAH,6.2/LIR

SMGs (z~2) BzKs (z~1.5) 70µm-selected (z~1) 24µm-selected (z=1-3) Local ULIRGs (z~0.07) 5MUSES IR galaxies (z~0.08)

10

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1010 1011 1012 1013 LIR (LO

  • )

0.001 0.010 LPAH,6.2/LIR

SMGs (z~2) BzKs (z~1.5) 70µm-selected (z~1) 24µm-selected (z=1-3) Local ULIRGs (z~0.07) 5MUSES IR galaxies (z~0.08)

10

Graciá-Carpio et al. 2011

Pope et al. 2013

Enhanced PAH emission at high redshift ... similar to enhanced [CII] emission?

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Pope et al. 2013

Link between enhanced PAH emission at high redshift and more molecular gas

1010 1011 1012 1013 LIR (LO

  • )

0.001 0.010 LPAH,6.2/LIR

SMGs (z~2) BzKs (z~1.5) 70µm-selected (z~1) 24µm-selected (z=1-3) Local ULIRGs (z~0.07) 5MUSES IR galaxies (z~0.08)

10 100 LIR/L’CO(1-0) [LO

  • / (K km s-1pc2)]
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Pope et al. 2013; Kirkpatrick, Pope, et al., 2014, ApJ submitted

1010 1011 1012 1013 LIR (LO

  • )

0.001 0.010 LPAH,6.2/LIR

SMGs (z~2) BzKs (z~1.5) 70µm-selected (z~1) 24µm-selected (z=1-3) Local ULIRGs (z~0.07) 5MUSES IR galaxies (z~0.08)

10 100 LIR/L’CO(1-0) [LO

  • / (K km s-1pc2)]

Link between enhanced PAH emission at high redshift and more molecular gas

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Pope et al. 2013

Link between enhanced PAH emission at high redshift and more molecular gas

Hollenbach & Tielens 1997

1010 1011 1012 1013 LIR (LO

  • )

0.001 0.010 LPAH,6.2/LIR

SMGs (z~2) BzKs (z~1.5) 70µm-selected (z~1) 24µm-selected (z=1-3) Local ULIRGs (z~0.07) 5MUSES IR galaxies (z~0.08)

10 100 LIR/L’CO(1-0) [LO

  • / (K km s-1pc2)]

10

Add [CII] to the mix

ALMA!

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Session: Star F Forma mation a n and nd A Assemb mbly o ly of Ga Gala laxies

! 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?

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! 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 LIR). Decompose IR SED to get the only the LIR,SF heated by SF. LMT pilot study:

  • Reduces the scatter in S-K
  • Brings more galaxies down onto the normal galaxy sequence

Session: Star F Forma mation a n and nd A Assemb mbly o ly of Ga Gala laxies

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! Are the measurements from different tracers of ISM and SF

consistent? How do galaxies grow (evolve) over cosmic time?

  • Strong PAH emission is much more prevalent at high redshift

compared to locally

  • Enhanced PAH emission is linked to the increased molecular gas

in high redshift galaxies

  • Future: add links to [CII] and other ISM tracers using ALMA

Session: Star F Forma mation a n and nd A Assemb mbly o ly of Ga Gala laxies

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Synergy between ALMA and LMT

50 m LMT [~2016] = 1/3 the collecting area

  • f ALMA
  • Wide field mm

mapping

  • Wide bandwidth

CO redshift surveys

EARLY SCIENCE WITH THE LARGE MILLIMETER TELESCOPE: EXPLORING THE EFFECT OF AGN ACTIVITY ON THE RELATIONSHIPS BETWEEN MOLECULAR GAS, DUST, AND STAR FORMATION

Allison Kirkpatrick1, Alexandra Pope1, Itziar Aretxaga2, Lee Armus3, Daniela Calzetti1, George Helou4, Alfredo Monta˜ na2, Gopal Narayanan1, F. Peter Schloerb1, Yong Shi5, Olga Vega2, Min Yun1

Draft version July 12, 2014

Submitted to ApJ July 12, 2014