J/A+A/673/A87 Molecular gas in superspiral galaxies (Lisenfeld+, 2023)
Molecular gas in superspiral galaxies.
Lisenfeld U., Ogle P.M., Appleton P.N., Jarrett T.H., Moncada-Cuadri B.M.
<Astron. Astrophys. 673, A87 (2023)>
=2023A&A...673A..87L 2023A&A...673A..87L (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, IR ; Interstellar medium ; Carbon monoxide
Keywords: galaxies: evolution - galaxies: ISM - galaxies: spiral -
ISM: molecules
Abstract:
At the highest stellar masses (log(M*)≳11.5M☉), only a small
fraction of galaxies are disk-like and actively star-forming objects.
These so-called `super spirals' are ideal objects to better understand
how galaxy evolution proceeds and to extend our knowledge about the
relation between stars and gas to a higher stellar mass regime. We
present new CO(1-0) data for a sample of 46 super spirals and for 18
slightly lower-mass (log((M*)>11.0M☉) galaxies with broad HI
lines -- HI fast-rotators (HI-FRs). We analyze their molecular gas
mass, derived from CO(1-0), in relation to their star formation rate
(SFR) and stellar mass, and compare the results to values and scaling
relations derived from lower-mass galaxies. We confirm that super
spirals follow the same star-forming main sequence (SFMS) as
lower-mass galaxies. We find that they possess abundant molecular gas
(mean redshift-corrected molecular gas mass fraction
(log(fmol,zcorr)=-1.36±0.02), which lies above the extrapolation
of the scaling relation with stellar mass derived from lower-mass
galaxies, but within the relation between fmol and the distance to
the SFMS. The molecular gas depletion time, τdep=Mmol/SFR, is
higher than for lower-mass galaxies on the SFMS
(τdep=9.30±0.03, compared to τdep=9.00±0.02 for the
comparison sample) and seems to continue an increasing trend with
stellar mass. HI-FR galaxies have an atomic-to-molecular gas mass
ratio that is in agreement with that of lower-mass galaxies,
indicating that the conversion from the atomic to molecular gas
proceeds in a similar way. We conclude that the availability of
molecular gas is a crucial factor to enable star formation to continue
and that, if gas is present, quenching is not a necessary destiny for
high-mass galaxies. The difference in gas depletion time suggests that
the properties of the molecular gas at high stellar masses are less
favorable for star formation.
Description:
We present and analyze CO(1-0) observations of a sample of 46 super
spiral (SS) galaxies, that is to say very massive
(log(M*)≳11.5M☉), actively star-forming disk galaxies. In
addition, we include a sample of somewhat less massive disk galaxies
with data for the atomic hydrogen and very broad HI spectra from
ALFALA (HI fast rotator HI galaxies, HI-FR).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 57 92 Velocity-integrated CO intensities
(central pointings)
table2.dat 61 92 Extrapolated molecular gas mass
table4.dat 148 92 WISE fluxes and classification
(corrected version, 24-Oct-2023)
table5.dat 57 64 Measured GALEX NUV flux and photometric errors,
SFR and stellar mass
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See also:
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
J/ApJS/243/14 : The Ogle et al. Galaxy Catalog (OGC) (Ogle+, 2019)
J/ApJS/233/22 : xCOLD GASS catalog (Saintonge+, 2017)
J/MNRAS/476/875 : xGASS catalog (Catinella+, 2018)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Name of the galaxy
22- 25 F4.2 mK rms Root-mean-square noise of the
CO(1-0) spectrum
30 A1 --- l_ICO10 Upper limit flag on ICO10
33- 37 F5.2 K.km/s ICO10 Velocity integrated intensity of the
CO(1-0) spectrum
43- 46 F4.2 K.km/s e_ICO10 ?=- Error of the velocity integrated
intensity of the CO(1-0) spectrum
49 I1 --- detICO10 [0/2] Detetction code for CO(1-0) (1)
54- 57 I4 km/s dVCO10 Zero-level line width of the CO(1-0) spectrum
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Note (1): Detetction code for CO(1-0) as follows:
0 = detection (ICO10/e_ICO10≥5)
1 = non-detection (ICO10/e_ICO10<3)
2 = tentative detection (3≤ICO10/e_ICO10<5)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Name of the galaxy
23- 27 F5.3 --- z Redshift, from SDSS DR9 or SR13
31- 34 I4 Mpc Dlum Luminosity distance
38 A1 --- l_logMmol Upper limit flag on logMmol
41- 45 F5.2 [Msun] logMmol Decimal logarithm of the
extrapolated molecular gas mass
50- 53 F4.2 [Msun] e_logMmol ?=- Error of the decimal logarithm of the
extrapolated molecular gas mass
58- 61 F4.2 --- faper Aperture correction
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Name of the galaxy
23- 28 F6.2 mJy FW1obs Observed flux in WISE band 1
32- 35 F4.2 mJy e_FW1obs Error of observed flux in WISE band 1
37- 42 F6.2 mJy FW1kcorr K-corrected flux in WISE band 1
47- 50 F4.2 mJy e_FW1kcorr Error of k-corrected flux in WISE band 1
53- 57 F5.2 mJy FW2obs Observed flux in WISE band 2
62- 65 F4.2 mJy e_FW2obs Error of observed flux in WISE band 2
69- 73 F5.2 mJy FW2kcorr K-corrected flux in WISE band 2
78- 81 F4.2 mJy e_FW2kcorr Error of k-corrected flux in WISE band 2
85- 89 F5.2 mJy FW3obs Observed flux in WISE band 3
94- 97 F4.2 mJy e_FW3obs Error of observed flux in WISE band 3
100-105 F6.2 mJy FW3kcorr K-corrected flux in WISE band 3
109-112 F4.2 mJy e_FW3kcorr Error of k-corrected flux in WISE band 3
114-119 F6.2 mJy FW4obs Observed flux in WISE band 4
123-127 F5.2 mJy e_FW4obs Error of observed flux in WISE band 4
130-135 F6.2 mJy FW4kcorr K-corrected flux in WISE band 4
140-143 F4.2 mJy e_FW4kcorr Error of k-corrected flux in WISE band 4
146-148 A3 --- CodeType [SS HI AGN] Code for galaxy type (1)
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Note (1): Code for galaxy type as follows:
SS = Super spiral
HI = HI fast rotator
AGN = AGN dominated galaxy
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 17 A17 --- Name Name of the galaxy
23- 28 F6.1 uJy FNUV ?=- NUV flux
33- 36 F4.1 uJy e_FNUV ?=- Error of NUV flux
40 A1 --- l_logSFR Upper limit flag on logSFR
44- 48 F5.2 [Msun/yr] logSFR Decimal logarithm the star formation rate
(SFR)
53- 57 F5.2 [Msun] logMstar Decimal logarithm the stellar mass
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Acknowledgements:
Ute Lisenfeld, ute(at)ugr.es
History:
25-Aug-2023: on-line version
24-Oct-2023: corrected table4 (from author)
(End) Patricia Vannier [CDS] 30-Mar-2023