J/ApJS/252/29 BAT AGN Spectroscopic Survey. XX. Molecular gas (Koss+, 2021)
BAT AGN Spectroscopic Survey.
XX. Molecular gas in nearby hard-X-ray-selected AGN galaxies.
Koss M.J., Strittmatter B., Lamperti I., Shimizu T., Trakhtenbrot B.,
Saintonge A., Treister E., Cicone C., Mushotzky R., Oh K., Ricci C.,
Stern D., Ananna T.T., Bauer F.E., Privon G.C., Bar R.E., De Breuck C.,
Harrison F., Ichikawa K., Powell M.C., Rosario D., Sanders D.B.,
Schawinski K., Shao Li, Megan Urry C., Veilleux S.
<Astrophys. J. Suppl. Ser., 252, 29 (2021)>
=2021ApJS..252...29K 2021ApJS..252...29K
ADC_Keywords: Active gal. nuclei; Carbon monoxide; Redshifts; Molecular data;
Surveys; Galaxies, Seyfert
Keywords: Active galactic nuclei ; AGN host galaxies ; Molecular gas ; Surveys ;
X-ray active galactic nuclei ; Survival analysis ;
Submillimeter astronomy ; High energy astrophysics ;
Seyfert galaxies ; Catalogs
Abstract:
We present the host-galaxy molecular gas properties of a sample of 213
nearby (0.01<z<0.05) hard-X-ray-selected active galactic nucleus (AGN)
galaxies, drawn from the 70-month catalog of Swift's Burst Alert
Telescope (BAT), with 200 new CO(2-1) line measurements obtained with
the James Clerk Maxwell Telescope and the Atacama Pathfinder
Experiment telescope. We find that AGN in massive galaxies
(log(M*/M☉)>10.5) tend to have more molecular gas and higher
gas fractions than inactive galaxies matched in stellar mass. When
matched in star formation, we find AGN galaxies show no difference
from inactive galaxies, with no evidence that AGN feedback affects the
molecular gas. The higher molecular gas content is related to AGN
galaxies hosting a population of gas-rich early types with an order of
magnitude more molecular gas and a smaller fraction of quenched,
passive galaxies (∼5% versus 49%) compared to inactive galaxies. The
likelihood of a given galaxy hosting an AGN (Lbol>1044erg/s)
increases by ∼10-100 between a molecular gas mass of 108.7M☉
and 1010.2M☉. AGN galaxies with a higher Eddington ratio
(log(L/LEdd)>-1.3) tend to have higher molecular gas masses and gas
fractions. The log(NH/cm-2)>23.4) of AGN galaxies with higher column
densities are associated with lower depletion timescales and may
prefer hosts with more gas centrally concentrated in the bulge that
may be more prone to quenching than galaxy-wide molecular gas. The
significant average link of host-galaxy molecular gas supply to
supermassive black hole (SMBH) growth may naturally lead to the
general correlations found between SMBHs and their host galaxies, such
as the correlations between SMBH mass and bulge properties, and the
redshift evolution of star formation and SMBH growth.
Description:
Our AGN parent sample consists of 836 ultrahard-X-ray-selected
(14-195keV) AGN included in the 70-month Swift-BAT all-sky catalog
(Baumgartner+ 2013, J/ApJS/207/19).
In total, 200 AGN galaxies were newly observed: 165 with the Atacama
Pathfinder Experiment (APEX) and 35 with the James Clerk Maxwell
Telescope (JCMT), while 13 were obtained from the literature
(see col. Tel in table 2 and Section 2.1.3).
The APEX 12m antenna observations totalled 254hr with 2288 400s long
scans, taken over 67 days between 2016 March and 2017 September. The
observing programs involved were mainly an ESO Large program
(PI M. Koss, ∼150hr), a follow-up ESO program (PI B. Trakthenbrot,
∼50hr), and Chilean time (PI E. Treister, ∼75hr). In addition to our
own programs, we also reduced data from archival programs for six BAT
AGN galaxies.
We observed the CO(2-1) transition (vrest=230.538GHz) using the
Swedish Heterodyne Facility Instrument (SHFI) with the eXtended Fast
Fourier Transform Spectrometer (XFFTS) backend (213-275GHz).
JCMT observations of the CO(2-1) molecular line were taken between
2011 February and 2013 April. Archival data for one additional galaxy
were also reduced (NGC 6240). We used the A3 (211-279GHz) receiver
with the ACSIS spectrometer with a beam size of 20.4" HPBW.
The results for the complementary sample of z<0.01 BAT AGN galaxies
are presented in Rosario+ (2018MNRAS.473.5658R 2018MNRAS.473.5658R).
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 108 213 Multiwavelength properties of the BAT AGN galaxy
sample
table2.dat 103 213 Catalog of CO(2-1) measurements
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See also:
B/swift : Swift Master Catalog (HEASARC, 2004-)
VII/258 : Quasars and Active Galactic Nuclei (13th Ed.) (Veron+ 2010)
J/ApJS/146/353 : Circumnuclear dust in galaxies (Martini+, 2003)
J/AJ/136/2782 : Star formation efficiency in nearby galaxies (Leroy+, 2008)
J/ApJ/701/587 : HST H-band imaging survey. II. QUEST QSOs (Veilleux+, 2009)
J/MNRAS/413/813 : ATLAS3D project. I. (Cappellari+, 2011)
J/ApJ/739/57 : Ultra hard X-ray AGNs in the Swift/BAT survey (Koss+, 2011)
J/MNRAS/415/32 : COLD GASS survey (Saintonge+, 2011)
J/MNRAS/414/940 : ATLAS3D project. IV. (Young+, 2011)
J/MNRAS/421/1569 : Properties of 18286 SDSS radio galaxies (Best+, 2012)
J/ApJ/746/L22 : Dual AGNs in the nearby Universe (Koss+, 2012)
J/MNRAS/426/2601 : CO lines in luminous IR galaxies (Papadopoulos+, 2012)
J/A+A/541/A118 : AGN-Host Galaxy Connection (Povic+, 2012)
J/ApJS/207/19 : Hard X-ray survey from Swift-BAT 6yrs (Baumgartner+, 2013)
J/ApJ/765/L26 : Swift/BAT X-ray data from GOALS LIRGs (Koss+, 2013)
J/A+A/564/A65 : Cold gas data of Herschel Reference Survey (Boselli+, 2014)
J/ApJ/794/152 : PACS observations of Herschel-BAT sample (Melendez+, 2014)
J/ApJS/219/1 : Catalog of Type-1 AGNs from SDSS-DR7 (Oh+, 2015)
J/ApJ/815/L13 : Compton-thick AGNs from 70-month Swift/BAT (Ricci+, 2015)
J/MNRAS/458/2221 : ATLAS3D Project. XXXI (Nyland+, 2016)
J/MNRAS/457/2703 : Local SDSS galaxies in Herschel Stripe 82 (Rosario+, 2016)
J/MNRAS/456/3335 : SPIRE observations of Herschel-BAT sample (Shimizu+, 2016)
J/A+A/604/A53 : ALLSMOG final DR. A new APEX CO survey (Cicone+, 2017)
J/ApJ/835/74 : IR phot. of AGNs in Swift/BAT 70 month (Ichikawa+, 2017)
J/ApJ/850/74 : Swift/BAT AGN Spectroscopic Survey. I. (Koss+, 2017)
J/ApJS/233/17 : Swift/BAT AGN spectroscopic survey. V. X-ray (Ricci+, 2017)
J/ApJS/233/22 : xCOLD GASS catalog (Saintonge+, 2017)
J/MNRAS/466/3161 : AGN global star-forming properties (Shimizu+, 2017)
J/A+A/609/A9 : Local Swift-BAT AGN observed with Herschel (Lutz+, 2018)
J/ApJ/870/31 : BAT AGN spectroscopic survey. XI. IR phot. (Ichikawa+, 2019)
J/ApJ/881/154 : BAT AGN spectroscopic survey. XVI. Blazars (Paliya+, 2019)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT [1/1413] Catalog ID in the BAT survey
6- 28 A23 --- Name Galaxy Name, optical/IR counterpart to AGN
30- 38 F9.5 deg RAdeg [0.2/352.3] Counterpart Right Ascension (J2000)
40- 48 F9.5 deg DEdeg [-78.9/63.7] Counterpart declination (J2000)
50- 58 A9 --- Type AGN type
60- 65 F6.4 --- zspec [0.01/0.05] Redshift (1)
67- 70 F4.1 arcsec rk20fe [5/82] Isophotal radius (2)
72- 73 I2 deg Incl [18/89] Inclination angle (3)
75- 84 A10 --- Morph Morphological classification (4)
86- 90 F5.2 [Msun] logM* [9.4/11.4] log of stellar masses of the
BAT AGN host galaxies (5)
92- 92 A1 --- l_SFR Limit flag on SFR
94- 99 F6.2 Msun/yr SFR [0/132]? Star formation rate (6)
101-101 A1 --- l_D(MS) Limit flag on DMS
103-108 F6.2 --- D(MS) [-10.3/2.2]? Offset from the Main Sequence
of star-formation (7)
--------------------------------------------------------------------------------
Note (1): Measurements from BASS/DR1, Koss+ (2017, J/ApJ/850/74) and
DR2 (Oh et al., in prep), when available. The redshift is based on
optical emission-line fitting (mainly of [OIII]5007Å). While the
emission line redshifts may have an offset from the systemic host
velocities, Rojas+ (2020MNRAS.491.5867R 2020MNRAS.491.5867R), they provide a rough
estimate of the likely CO centroid.
Note (2): The isophotal radius at a surface brightness of 20mag/arcsec2 in
the K-band, taken from the 2MASS extended source catalog,
Jarrett+ (2000AJ....119.2498J 2000AJ....119.2498J).
Note (3): Galaxy inclination angle based on r-band optical imaging from the
SDSS, Kitt Peak (Koss+ 2011, J/ApJ/739/57), or from the 2MASS extended
source catalog (Jarrett+ 2000AJ....119.2498J 2000AJ....119.2498J). In order to determine
the inclination from the observed ratio of the semi-minor to
semi-major axes of the galaxy, we use the prescription of
Davis+ (2011MNRAS.414..968D 2011MNRAS.414..968D) for both early and late-type galaxies.
Note (4): Morphological classification from Galaxy Zoo
(Lintott+ 2008MNRAS.389.1179L 2008MNRAS.389.1179L), when available, followed by the Third
Reference Catalog of Bright Galaxies (RC3, de Vaucouleurs+ 1995, VII/155),
and finally visual inspection following the approach of
Koss+ (2011, J/ApJ/739/57), which is based on optical imaging.
Values can be "elliptical", "spiral", or "uncertain". See Appendix A
for a further discussion of uncertainty in morphology measures.
Note (5): Stellar masses of the BAT AGN host galaxies. We combined near-IR
data from 2MASS, which is more sensitive to stellar emission, with
mid-IR data from the AllWISE catalog (II/328), which is more sensitive
to AGN emission (i.e., re-processed by the circumnuclear dusty gas).
See Powell+ (2018ApJ...858..110P 2018ApJ...858..110P) for a further description of these
measurements.
Note (6): The majority (80%, 171/213) of SFR estimates were derived from the
Herschel-based study of BAT AGN galaxies by
Shimizu+ (2017, J/MNRAS/466/3161), which measured the total IR
(8-1000um) luminosities by decomposing the IR SEDs into AGN- and
galaxy-related components using WISE (3.4, 4.6, 12, and 22um),
Herschel PACS (70 and 160um) and SPIRE (250, 350, and 500um) imaging.
A subset of 19% (40/213) AGN galaxies were not part of this Herschel
imaging publication. For these we adopt the results of
Ichikawa+ (2019, J/ApJ/870/31), who performed a similar IR SED
decomposition but included any available WISE, Akari, IRAS, and
Herschel measurements. See Appendix B for a further discussion about
uncertainties and offsets in SFR measurements.
Note (7): The offset, D(MS), is defined as the difference on a logarithmic
scale between the observed SFR of a galaxy and it's expected SFR in
relation to the MS from Renzini & Peng (2015ApJ...801L..29R 2015ApJ...801L..29R).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT [1/1413] Catalog ID in the BAT
survey
6- 28 A23 --- Name Galaxy Name, optical/IR
counterpart to AGN
30- 33 A4 --- Tel Telescope used for the CO
observation (1)
35- 36 I2 arcsec HPBW [20/32] Associated beam size
38 I1 --- FlagCO21 [0/1] Detection flag for the
CO(2-1) line (1=detection) (2)
40- 43 F4.1 mK sigma-CO21 [0.4/17.1]? RMS noise achieved
around the CO(1-0) line (3)
45- 48 F4.2 --- C-aper [1.0/8.71] Beam correction
factor (4)
50- 53 F4.1 --- SN-inte [-3/39.5] Signal-to-noise,
integrated line
55- 59 F5.1 10+8K.km/s.pc2 L-inte [0.2/105.5] Total CO(2-1) line
luminosity from integrated
line (5)
61- 65 F5.2 [Msun] logMH2 [8/10.7] Log of total molecular gas
mass (6)
67- 71 F5.2 [yr] logtdepH2 [7.5/20.1]? Log of gas depletion
timescale (7)
73- 74 I2 --- Pro [-1/2]? Fit type (8)
76- 80 F5.1 10+8K.km/s.pc2 L-pro [0.2/132.1]? Total CO(2-1) line
luminosity from the profile
fit (9)
82- 85 F4.1 --- SN-pro [1.5/55.1]? Signal-to-noise, CO
profile
87- 89 I3 km/s W50 [41/658]? FWHM of the CO line
from profile fit
91- 93 I3 km/s e_W50 [18/953]? Uncertainty in W50
95- 99 I5 km/s zCO [3151/14928]? Redshift from the
central CO velocity
101- 103 I3 km/s e_zCO [2/327]? Uncertainty in zCO
--------------------------------------------------------------------------------
Note (1): Telescope as follows:
APEX = APEX 12m antenna observations from our and archival ESO programs
(165 occurrences; see the "Description" section above)
JCMT = Our 35 JCMT/ACSIS spectrometer observations and two archival data
published in Papadopoulos+ 2012, J/MNRAS/426/2601
(see the "Description" section above)
CSO = Caltech Submillimeter Observatory, HPBW=32"
from Monje+ 2011ApJS..195...23M 2011ApJS..195...23M (5 occurrences)
IRAM = IRAM from Bertram+ 2007A&A...470..571B 2007A&A...470..571B with the CO(1-0) line (HPBW=22")
instead of CO(2-1) line (4 occurrences)
SEST = The 15m Swedish ESO Sub-millimeter Telescope (HPBW=23" at 230GHz)
published in Strong+ 2004MNRAS.353.1151S 2004MNRAS.353.1151S (2 occurrences)
Note (2): A detection flag for the CO(2-1) line. In the cases where the
line is not detected ("0"), the tabulated line luminosities and
molecular gas masses are 3σ upper limits.
Note (3): RMS noise achieved around the CO(1-0) line, in spectral channels
with width Δwch=50km/s. The quoted RMS is at 50km/s even for
spectra with finer binning.
Note (4): Beam aperture correction, derived either through simulations
following the approach developed for the COLD GASS sample
(Saintonge+ 2011, J/MNRAS/415/32), or by assuming the CO luminosity is
traced by the 160um emission observed by Herschel/PACS (FWHM=12"), as
reported by Melendez+ (2014, J/ApJ/794/152).
Note (5): Total CO(2-1) line luminosity, calculated from the observed
CO(2-1) line luminosity and the aperture correction. The error includes
the measurement uncertainty, a 10% flux calibration error, and the 15%
uncertainty on the aperture correction (Saintonge+ 2011, J/MNRAS/415/32)
-- all combined in quadrature. If the source is undetected in CO
(FlagCO21=0 in Col. 3), then the tabulated value corresponds to a
3σ upper limit.
Note (6): Total molecular gas mass, including the Helium contribution,
calculated from the integrated CO(2-1) line luminosity assuming a
conversion of 0.79 from CO(2-1) to CO(1-0), and assuming a Milky
Way-like conversion factor of αCO=4.3M* (K.km/s.pc2)-1
(Bolatto+ 2013Natur.499..450B 2013Natur.499..450B). If the source is undetected in CO
(FlagCO21=0), then the tabulated value corresponds to a
3σ upper limit.
Note (7): The gas depletion timescale (tdep(H2)=MH2/SFR). A small
number (8%, 16/207) of AGN galaxies have no measurements (denoted as
blank or null values in the data table), since they lack robust SFR
measurements. Most of these (14/16) were not observed within the
Herschel program, and thus have less sensitive SFR upper limits, or
lie close to the Galactic plane where no measurements were performed
(12%, 2/16). Most are also undetected in molecular gas (75%, 12/16).
As they have upper limits on SFR and molecular gas, a gas depletion
timescale, which is the ratio of the two, cannot be estimated
Note (8): CO line measured with either a single (1) or double (2) peak
Gaussian profile (as indicated by W50type; Tiley+ 2016MNRAS.461.3494T 2016MNRAS.461.3494T).
Values of -1 indicate CO line fits from the literature.
Note (9): Total CO(2-1) line luminosity, calculated from the profile fit
L'pro,corr; corrected with an aperture correction.
--------------------------------------------------------------------------------
History:
From electronic version of the journal
References:
Koss et al. Paper I. 2017ApJ...850...74K 2017ApJ...850...74K Cat. J/ApJ/850/74
Berney et al. Paper II. 2015MNRAS.454.3622B 2015MNRAS.454.3622B
Oh et al. Paper III. 2017MNRAS.464.1466O 2017MNRAS.464.1466O
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(End) Prepared by [AAS], Emmanuelle Perret [CDS] 23-Apr-2021