J/A+A/628/A104 [ESS2003] Q2343-BX610 reduced PdBI spectra (Brisbin+, 2019)
Neutral carbon and highly excited CO in a massive star forming main sequence
galaxy at z=2.2.
Brisbin D., Aravena M., Daddi E., Dannerbauer H., Decarli R.,
Gonzalez Lopez J., Riechers D., Wagg J.
<Astron. Astrophys. 628, A104 (2019)>
=2019A&A...628A.104B 2019A&A...628A.104B (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, spectra ; Spectra, millimetric/submm
Keywords: galaxies: ISM - galaxies: star formation - galaxies: high-redshift -
submillimeter: galaxies - photon-dominated region
Abstract:
We have used the Plateau De Bure Interferometer to observe multiple CO
and neutral carbon transitions in a z=2.2 main sequence disk galaxy,
BX610. Our observation of CO(7-6), CO(4-3) and both far infrared [CI]
lines complements previous observations of H-alpha and low-J CO, and
reveal a galaxy that is vigorously forming stars with UV fields,
(Log(G/G0)<3.25), less extreme than local ULIRGs or most
starbursting submillimeter galaxies in the early universe. Our
observations allow new independent estimates of the cold gas mass
which indicate Mgas∼2x1011M☉, and suggest a modestly larger
alpha_CO value of ∼8.2. The corresponding gas depletion timescale is
∼1.5Gyr. In addition to gas of modest density (Log(n[cm-3])<3)
heated by star formation, BX610 shows evidence for a significant
second gas component responsible for the strong high-J CO emission.
This second component might either be a high density molecular gas
component heated by star formation in a typical photodissociation
region, or it could be molecular gas excited by low velocity C shocks.
The CO(7-6) to far infrared luminosity ratio we observe is
significantly higher than typical star forming galaxies and suggests
that CO(7-6) is not a reliable star formation tracer in this galaxy.
Description:
Reduced PdBI spectra for [ESS2003] Q2343-BX610 over three bands are
presented. These bands cover the CO(4-3), [CI](1-0), and CO(7-6) &
[CI](2-1) emission line transitions (the final two covered by a single
band). The data corresponds to that presented in Fig. 1 of the paper.
For each band, two columns are included. The first gives the
observed frequency (GHz), and the second gives flux density (mJy/beam)
of the peak pixel. These are the reduced spectra which were used for
calculating line fluxes. The spectra corresponding to CO(4-3) and
[CI](1-0) have been adjusted by a factor of 0.8 to account for a
discrepancy noted in the calibrator fluxes. Further observing and data
reduction details are discussed in sections two and three of paper.
Objects:
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RA (2000) DE Designation(s)
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23 46 09.43 +12 49 19.2 [ESS2003] Q2343-BX610 = [ESS2003] Q2343-BX610
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
co43.dat 21 109 CO(4-3) spectrum
ci10.dat 21 102 [CI](1-0) spectrum
250ghz.dat 21 69 Spectrum covering the CO(7-6) and [CI](2-1)
emission lines
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Byte-by-byte Description of file: 250ghz.dat ci10.dat co43.dat
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Bytes Format Units Label Explanations
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1- 7 F7.3 GHz Freq Observed frequency
16- 21 F6.3 mJy/beam Fdens Flux density
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Acknowledgements:
Drew Brisbin, brisbind(at)gmail.com
(End) Drew Brisbin [UDP, Chile], Patricia Vannier [CDS] 05-Jul-2019