Radio Spectroscopy A

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Radio spectroscopy A. Harris

Image: part of an H-ATLAS field as seen in the Herschel-SPIRE 250/350/500 m bands H-ATLAS: Eales et al., PASP 2010

Annoying question at a NSF Science and Technology Center Review “Are the graduate students being properly prepared to enter the 21st century job markt?”ket?” General, strong background: • Physics • Applied math • Computer science

Diverse and useful skills: • Computing (programming, modeling) • Instrumentation

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Key questions for radio astronomy

 Among the most important topics in radio astronomy are:  Structure in the Cosmic Microwave Background (power spectrum, polarization)  The era of galaxy formation . Finding the early galaxies . Investigating and understanding local templates  Star formation  Structure of molecular clouds  Structure of active and normal galactic nuclei

16 element scalable W-band focal plane array for the GBT

Argus is being commiiissione d on the GBT. It 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

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Large area mapping with Argus

 Spectral imaging in HCN, HCO+, 13CO, C18O . Dense regions . Column densities  GlGalac tic an d extragalactic star formation . GlGalac tifiltic filamen ts . Extragalactic GMCs . Galactic center . Extragalactic nuclei

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The 100 meter Green Bank Telescope National Radio Astronomy Observatory Green Bank Observatory (GBO) Green Bank, West Virginia

GBT photo

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The view from the top

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Stratospheric Observatory SOFIA PUdtProgram Update StratosphericfIfdAtfor Infrare Observatoryd Astronomy for Infrared Astronomy (SOFIA) SOFIA Splinter Meeting, AAS, Pasadena 7 June 2009

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Galactic Center in radio continuum

VLA image

What warms the dense molecular material in the Galactic center?

 Center molecular clouds are substantially warmer than disk clouds (e.g. Güsten+85)  Lots of energy available: a black hole, hot stars (UV), intersecting orbits and colliding stellar winds (shocks), X-rays, rigid magnetic fie lds, radi o lo bes… A pretty active nucleus  A galactic nucleus we can undtdidtilderstand in detail At 8.3 kpc, 10” = 0.4 pc

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[N II] and [O III] in the Arches 6 rris+201 Ha Green circle diameter  MSX point source catalog 8µm/24µm

[O III]/[N II] in J02399-0136 and in the Galactic center Arches

Arches: Sickle: 35500 K 36200 K

HII: Rubin 85, by Fkihff11

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A solution?

Cluster of  Geometrical dilution Cloud boundary can’t change field early O, hardness WR stars  No O stars? Unlikely. [O III]  But: density gradient at 35-55 eV cloud edge can soften radiation field with distance into cloud, [N II] reducing apparent 14-30 eV [O III]/[NII] ratio  Test with SOFIA FIFI-LS [N III] observations scheduled for summer Radio cont. 2016: does [N II] have 13.6 eV same spatial distribution as [O III] or as [N II]? In 2 d  e

FIFI-LS footprints on the Galactic Center’s Sickle and Arches

Color Herschel-PACS [N II]; contours 20 cm radio continuum

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Universe’s structure formation

Cosmic star formation rate density vs. redshift

Carilli & Walter 2013, after Bouwens et al. 2010

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The Zpectrometer ultrawideband correlation spectrometer NSF ATI Program award AST-0503946 to UMD

The 100 meter diameter Robert C. UMD’s Zpectrometer correlators on the Byrd Green Bank Telescope (GBT) GBT receiver turret

COMAP survey properties at z ~ 2.9

 Sensitive to clusters of galaxies  10 m telescope, 26-34 GHz; 29 GHz center f req uenc y, ~3 .4’ beam  Beam size corresponds to a comoving ~6 Mpc  z ~ 0.006 matches the linear and line of sight scales  This corresponds to f ~ 48 MHz, or ~165 “slices” in an 8 GHz bandwidth (covering ~1 Gyr)  Comoving volume of ~600 Mpc3 for each “slice” (each covering ~60 Myr)

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Simulated integrated intensity images

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Cross-correlation distinguishes signal from noise

Potential projects  HhlHIFIdSOFIAGltit(dtHerschel HIFI and SOFIA Galactic center (data analysis; with MPIfR Bonn, UCLA, Cornell). A great second-year project.  Argus obdffbservations and mapping software for the GBT: dense gas mapping of galaxies and galactic filaments at 4 mm wavelength (With BltttBoltattoor Md)Mundy)  COMAP CO integrated intensity experiment to trace star formation near the peak of the galflaxy forma tidtion and mass assem bly era (High risk, high gain in a big international project)