J/A+A/658/A124 CO-CAVITY pilot survey. CO spectra (Dominguez-Gomez+, 2022)
The CO-CAVITY pilot survey: Molecular gas and star formation in void galaxies.
Dominguez-Gomez J., Lisenfeld U., Perez I., Lopez-Sanchez A.R.,
Duarte Puertas S., Falcon-Barroso J., Kreckel K., Peletier R.F.,
Ruiz-Lara T., van de Weygaert R., van der Hulst J.M., Verley S.
<Astron. Astrophys. 658, A124 (2022)>
=2022A&A...658A.124D 2022A&A...658A.124D (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, nearby ; Galaxies, radio ; Photometry, millimetric/submm
Keywords: ISM: molecules - ISM: atoms - galaxies: star formation -
Galaxy: evolution - large-scale structure of Universe -
radio lines: galaxies
Abstract:
Voids are the most under-dense large-scale regions in the Universe.
Galaxies inhabiting voids are one of the keys to understand the
intrinsic processes of galaxy evolution, as external factors such as
multiple galaxy mergers or a dense self-collapsing environment are
negligible.
We present the first molecular gas mass survey of void galaxies. We
compare these new data, together with data for the atomic gas mass
(MHI) and star formation rate (SFR) from the literature to those of
galaxies in filaments and walls in order to better understand how
molecular gas and star formation are related to the large-scale
environment.
We observed at the IRAM 30-m telescope the CO(1-0) and CO(2-1)
emission of 20 void galaxies selected from the VoidGalaxy Survey
(VGS), with a stellar mass range from 108.5to 1010.3M. We detected 15
objects in at least one CO line. We compare the molecular gas mass
(MH2), the star formation efficiency (SFE=SFR/MH2), the atomic gas
mass, the molecular-to-atomic gas-mass ratio, and the specific star
formation rate (sSFR) of the void galaxies with two control samples of
galaxies in filaments and walls,selected from xCOLD GASS and
EDGE-CALIFA, for different stellar mass bins and taking the star
formation activity into account.
In general, we do not find any significant differences between void
galaxies and the control sample. In particular, we do not find any
evidence for a difference in the molecular gas mass or molecular gas
mass fraction. Also for the other parameters (SFE,atomic gas mass,
molecular-to-atomic gas mass ratio, and sSFR) we find similar (within
the errors) mean values between void, and filament and wall galaxies
when limiting the sample to star-forming galaxies. We find no evidence
for an enhanced sSFR in void galaxies. Some tentative differences
emerge when studying trends with stellar mass: The SFE of void
galaxies might be lower than in filament and wall galaxies for low
stellar masses, and there might be a trend of increasing deficiency in
the HI content in void galaxies compared to galaxies in filaments and
walls for higher stellar masses, accompanied by an increase in the
molecular-to-atomic gas-mass ratio. However, all trends with stellar
mass are based on a low number of galaxies and need to be confirmed
for a larger sample.
The results for the molecular gas mass for a sample of 20 voids
galaxies allowed us, for the first time, to make a statistical
comparison to galaxies in filaments and walls. We do not find any
significant differences of the molecular gas properties and the SFE,
but we note that a larger sample is necessary to confirm this and be
sensitive to subtle trends.
Description:
Here we provide the CO(1-0) and CO(2-1) spectra of 20 void galaxies
from the Void Galaxy Survey (VGS, Kreckel et al. 2012AJ....144...16K 2012AJ....144...16K,
Cat. J/AJ/144/16) gathered with the IRAM-30m telescope, see Appendix
C).
For each galaxy and line, we list the observed frequency (in MHz) and
intensity of the spectra (in the main beam temperature scale, in units
of K, baseline subtracted).
The file names with the spectra indicate the name of the galaxy and
the emission line. For instance, "VGS11CO10.dat" is the CO(1-0)
emission line spectra of the galaxy VGS_11, and "VGS04CO10.dat" is
the CO(2-1) emission line spectra of galaxy VGS_04.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
sources.dat 53 20 List of studied galaxies
sp/* . 40 Individual spectra
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See also:
J/AJ/144/16 : Optical and HI properties of galaxies in voids (Kreckel+, 2012)
Byte-by-byte Description of file: sources.dat
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Bytes Format Units Label Explanations
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1- 7 A7 --- Name Galaxy name
11- 12 I2 h RAh Simbad right ascension (J2000)
14- 15 I2 min RAm Simbad right ascension (J2000)
17- 21 F5.2 s RAs Simbad right ascension (J2000)
23 A1 --- DE- Simbad declination sign (J2000)
24- 25 I2 deg DEd Simbad declination (J2000)
27- 28 I2 arcmin DEm Simbad declination (J2000)
30- 33 F4.1 arcsec DEs Simbad declination (J2000)
37- 53 A17 --- SName Simbad name
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Byte-by-byte Description of file: sp/*
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Bytes Format Units Label Explanations
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3- 12 F10.3 MHz Freq Observed frequency
16- 23 F8.5 K Tmb Mean beam temperature
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Acknowledgements:
Jesus Dominguez Gomez, jesusdg(at)ugr.es,
Universidad de Granada, Spain
(End) J. Dominguez Gomez [Univ. Granada, Spain], P. Vannier [CDS] 13-Nov-2021