Frayer ( 1) Redshifted Molecular Gas – Evolution of Galaxies David T. Frayer (NRAO) ALMA-Band2 2013 ALMA Band-2 (68-90 GHz) is a crucial missing band for astronomy. Before the GBT 4mm system, there was very limited sensitivity coverage below 80 GHz. http://www.gb.nrao.edu/4mm/
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Frayer (1) Redshifted Molecular Gas – Evolution of Galaxies David T. Frayer (NRAO) ALMA-Band2 2013 ALMA Band-2 (68-90 GHz) is a crucial missing band for.
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Frayer (1)
Redshifted Molecular Gas – Evolution of Galaxies
David T. Frayer (NRAO)
ALMA-Band2 2013
ALMA Band-2 (68-90 GHz) is a crucial missing band for astronomy.
Before the GBT 4mm system, there was very limited sensitivity coverage below 80 GHz. http://www.gb.nrao.edu/4mm/
Frayer (2)
ALMA Band-2 (4mm Rx) “Key Science”
• Fundamental Physics – With VLBI, probe the physics near the base of black hole jets in nearby galaxies {and measure the size of the galaxy via parallax of SagA*}.
• The Context of Star Formation – Deuterium species and dense gas tracers key for studies of cold cloud cores from which stars form.
• Origin of Life – Complex organic molecules and pre-biotic molecules in the ISM and comets which are key for studying the conditions from which life eventually forms (unexplored frequencies --- lots of discovery potential in astro/bio-chemistry).
• Galaxies Across Cosmic Time – CO(1-0) at intermediate redshifts where the evolution of galaxies is proceeding rapidly and dense gas tracers, such as HCN and HCO+, in local star-forming galaxies.
Intermediate redshift galaxies and (1-0) transitions are important for understanding galaxy evolution
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Star-Formation History from the Infrared
ALMA-Band2 2013
Magnelli, et al. 2009 (Spitzer FIDEL-70um result)
Why are LIRGs important?The bulk of the infrared EBL is at z~1, and the rapid evolution from now to z~1 is associated luminous infrared star-forming galaxies (LIRGs). Herschel and Spitzer Surveys found large numbers of z~0.2-1 LIRGS. CO at intermediate redshifts key.
ULIRGs
LIRGs
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HST imaging of local IRAS LIRGs (part of GOALS sample – Great Observatories All-sky LIRG Survey)
ALMA-Band2 2013
What are LIRGs?--Diverse systems of mergers and disks
GBT/Zpectrometer CO(1-0) and CARMA/PdBI CO(3-2) observations of Herschel SMGs show wide range of L’[CO](3-2/1-0) ratios of ~0.6+/-0.4 Need 1-0 line for molecular mass measurements.
Why CO(1-0)?
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VLA CO(1-0) Imaging
ALMA-Band2 2013
Observations suggest low-CO excitation for both the BzK’s and SMG samples extended cold CO(1-0)? Imaging: Extended emission or separated clumps, outflows, disks, structure/kinematics ALMA
BzKs (Aravena et al. 2010)
SMGs (Ivison et al. 2010):
Why do we need spatial resolution?
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Comparison of ALMA,VLA, and the GBT for redshifted CO(1-0)
ALMA-Band2 2013
Detection levels for same amount of observing time
Plot made in Aug 2012, before GBT 4mm upgrade
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Evolution Disks vs “Merger” Starbursts
ALMA-Band2 2013
Daddi et al. 2010b BzK’s and Tacconi et al. 2010 disk selected sample compared with the SMGs. With CO(1-0) at intermediate redshift, ALMA-Band-2 can study the molecular mass evolution of the “disk sequence” in the transition epoch between z~0--1.
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Dense Gas in Local Galaxies
ALMA-Band2 2013
Gao & Solomon 2004: Dense gas traced by HCN better correlated with Lir than CO. SFE correlated with dense gas fraction. HCN & HCO+
Frayer (11)ALMA-Band2 2013
Significant HCO+/HCN variations in starbursts and AGN sources, although tracing similar densities.
Kripps et al. 2008
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ALMA mapping CO, HCN, HCO+
• (HCN & HCO+)/CO measures dense gas fraction, star-formation efficiency
• HCN/CO strong enhancements AGN, extremely compact IR sources (x-ray heating, IR pumping)
• HCO+/HCN ratio enhanced in star-forming regions (UV-field, SN shocks)
ALMA-Band2 2013
Frayer (13)ALMA-Band2 2013
Frayer et al. 1999
Local example:VV114 merger system shows molecular gas and dust that peaks between the two main optical components. The mid-IR emission peaks on the extremely red J-K source in VV114 East
Frayer (14)ALMA-Band2 2013 Imanishi et al. 2007
HCO+ peaks on the star-forming regions with the CO and dust between VV114E&W, while HCN peaks on the strong mid-IR/extremely red VV114E component
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Variations of Molecular Lines in
Nearby Galaxies, e.g. IC342 Meier & Turner 2005
ALMA-Band2 2013
IC342: CO=green, HI=red
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16 element scalable W-band FPA for the GBT
ALMA-Band2 2013
Argus is scheduled to be deployed at the GBT by November 2014 and is a collaboration between Stanford U. (PI Sarah Church), Caltech, JPL, Univ. Maryland, Univ. Miami, and NRAO.
Frequency operation range: 75-115.3 GHz
Tsys~75K
Frayer (17)ALMA-Band2 2013
GBT (9”)1pixel
GBT/ARGUS16pixel
GBT100pixel
ALMA1”
ALMA5”
ACA(23”)
ALMA-TP (70”)
Rms=1mJy/beam per point
2.5min 2.5min 2.5min 1.2min 1.2min 5hr 3hr
Rms=2mKper point
2.5min 2.5min 2.5min 122hr 11min 6min 3s
Map 3’x3’with 1mJy/beam
18hr 69min 11min 59min 59min 80hr 27hr
Map 3’x3’ with 2mK
18hr 69min 11min 6000hr 9hr 96min 27s
GBT vs ALMA Sensitivity: Estimated Observing Times
Interferometers provide high-resolution data and good point-source sensitivity (mJy/beam), but lack sensitivity to extended emission (mK).
Frayer (18)ALMA-Band2 2013
CASA Simulations to compare GBT vs ALMA+ACA+ALMA_TP30dor 8um IRAC image – Rescaled from 2” pixels to 1” pixels.
30dor in the LMC is the most luminous star-formation region in the local group of galaxies.
Frayer (19)ALMA-Band2 2013
GBT simulated HCN image:
Total flux: 1.25 Jy
Contours are (0.05, 0.1, 0.2, 0.4, 0.6, 0.8) x peak.