J/ApJS/269/24 BASS. XXXIV. ALMA obs. of Swift/BAT AGNs (Kawamuro+, 2023)
BASS. XXXIV.
A catalog of the nuclear millimeter-wave continuum emission properties of AGNs
constrained on scales ≤100-200pc.
Kawamuro T., Ricci C., Mushotzky R.F., Imanishi M., Bauer F.E., Ricci F.,
Koss M.J., Privon G.C., Trakhtenbrot B., Izumi T., Ichikawa K.,
Rojas A.F., Smith K.L., Shimizu T., Oh K., den Brok J.S., Baba S.,
Balokovic M., Chang C.-S., Kakkad D., Pfeifle R.W., Temple M.J., Ueda Y.,
Harrison F., Powell M.C., Stern D., Urry M., Sanders D.B.
<Astrophys. J. Suppl. Ser., 269, 24 (2023)>
=2023ApJS..269...24K 2023ApJS..269...24K
ADC_Keywords: Active gal. nuclei; Millimetric/submm sources; Gamma rays;
X-ray sources; Redshifts
Keywords: Active galactic nuclei ; Millimeter astronomy ; Galactic center ;
High energy astrophysics ; Astrophysical black holes
Abstract:
We present a catalog of the millimeter-wave (mm-wave) continuum
properties of 98 nearby (z<0.05) active galactic nuclei (AGNs)
selected from the 70 month Swift/BAT hard-X-ray catalog that have
precisely determined X-ray spectral properties and
subarcsecond-resolution Atacama Large Millimeter/submillimeter Array
Band 6 (211-275GHz) observations as of 2021 April. Due to the
hard-X-ray (>10keV) selection, the sample is nearly unbiased for
obscured systems at least up to Compton-thick-level obscuration, and
provides the largest number of AGNs with high-physical-resolution
mm-wave data (≲100-200pc). Our catalog reports emission peak
coordinates, spectral indices, and peak fluxes and luminosities at
1.3mm (230GHz). Additionally, high-resolution mm-wave images are
provided. Using the images and creating radial surface brightness
profiles of mm-wave emission, we identify emission extending from the
central sources and isolated blob-like emission. Flags indicating the
presence of these emission features are tabulated. Among 90 AGNs with
significant detections of nuclear emission, 37 AGNs (∼41%) appear to
have both or one of extended or blob-like components. We, in
particular, investigate AGNs that show well-resolved mm-wave
components and find that these seem to have a variety of origins
(i.e., a jet, radio lobes, a secondary AGN, stellar clusters, a
narrow-line region, galaxy disk, active star formation regions, or
AGN-driven outflows), and some components have currently unclear
origins.
Description:
Our sample includes all nearby (z<0.05) 70 month BAT AGNs in
Baumgartner+ (2013, J/ApJS/207/19) with X-ray spectral properties
precisely determined by Ricci+ (2017, J/ApJS/233/17 ; Paper V) and
with subarcsecond-resolution Band 6 (211-275GHz) ALMA data taken at
high resolutions of ≲0.6", publicly available as of 2021 April. The
information on the ALMA data we analyzed is summarized in Table 2 in
Appendix A.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 97 98 Basic properties of our targets
table2.dat 98 106 Basic information of ALMA data
table3.dat 91 98 Complete list of mm-wave properties
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See also:
J/ApJS/95/1 : Atlas of Quasar Energy Distributions (Elvis+ 1994)
J/ApJS/103/81 : 1.425GHz atlas of IRAS bright galaxies. II. (Condon+, 1996)
J/A+A/495/691 : Multifreq. catalog of blazars, Roma-BZCAT (Massaro+, 2009)
J/ApJ/728/58 : Swift-BAT survey of AGNs (Burlon+, 2011)
J/ApJS/207/19 : Hard X-ray survey from Swift-BAT 6yrs (Baumgartner+, 2013)
J/ApJ/815/L13 : Compton-thick AGNs from 70-month Swift/BAT (Ricci+, 2015)
J/ApJ/822/109 : MIR view of polar dust emission in local AGNs (Asmus+, 2016)
J/ApJS/233/17 : Swift/BAT AGN spectroscopic survey. V. X-ray (Ricci+, 2017)
J/ApJ/835/223 : A catalog of nearby galaxies with Chandra obs. (She+, 2017)
J/ApJ/881/154 : BAT AGN spectroscopic survey. XVI. Blazars (Paliya+, 2019)
J/MNRAS/495/3943 : Hard-X-ray-selected AGNs I (Chiaraluce+, 2020)
J/A+A/633/A79 : NGC 6240 MUSE observations (Kollatschny+, 2020)
J/ApJ/910/104 : subarcsec MIR view of local AGN. IV. ISAAC (Isbell+, 2021)
J/ApJS/261/2 : BASS. XXII. Swift/BAT AGN Sp. Survey DR2 cat. (Koss+, 2022)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Seq [1/98] Identification number
4- 7 A4 --- Index BAT index in previous papers
9- 22 A14 --- SWIFT BAT name (JHHMM.m+DDMMAN)
from Ricci+ 2017, J/ApJS/233/17
24- 46 A23 --- CName Counterpart name from Ricci+ 2017, J/ApJS/233/17
48- 57 F10.6 deg RAdeg Right ascension in decimal degrees (J2000)
59- 68 F10.6 deg DEdeg Declination in decimal degrees (J2000)
70- 72 A3 --- Ref Reference for the position (1)
74- 80 F7.5 --- z [0.001/0.05] Redshift (2)
82- 86 F5.1 Mpc Dist [3.5/216] Distance (2) (3)
88- 91 F4.1 Mpc e_Dist [0.1/14] Uncertainty in Dist (2) (3)
93 A1 --- f_Dist [a] Flag on Dist (4)
95- 97 F3.1 --- Type [1.0/2.0] Seyfert type (2)
--------------------------------------------------------------------------------
Note (1): Reference as follows:
A = ALMA (this work);
W = ALLWISE (Wright+ 2010AJ....140.1868W 2010AJ....140.1868W --see II/328 ;
Mainzer+ 2011ApJ...731...53M 2011ApJ...731...53M);
CXO = Chandra (this work).
Note (2): Taken from the BASS DR2 paper of Koss+ (2022, J/ApJS/261/2)
or the authors.
Note (3): Particularly for objects at distances below 50Mpc,
redshift-independent distances are adopted by referring to the
Extragalactic Distance Database of Tully+ 2009AJ....138..323T 2009AJ....138..323T,
a catalog of the Cosmicflows project (Courtois+ 2017ApJ...847L...6C 2017ApJ...847L...6C),
and NASA/IPAC Extragalactic Database in this order (see
Koss+ 2022, J/ApJS/261/2 for details).
Note (4): Flag as follows:
a = A small redshift error of the order 10km/s, used in computing the
distance error, results in a very small error of ≪0.1Mpc and thus
0.1Mpc is denoted as a substitute.
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Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Seq [1/98] Identification number
4- 17 A14 --- Project ALMA project code
19- 35 A17 --- OUSID Member observation unit set (OUS) identifier
37- 42 A6 --- Mosaic Mosaic observation or not
("mosaic"=12 occurrences)
44- 48 F5.2 arcsec MRS [0.3/13.6]? Maximum recoverable scale (1)
50- 55 F6.2 arcsec FOV [21.9/227.1]? Field of view from ALMA archive
57- 61 I5 s Exp [65/19813]? Exposure from ALMA archive
63- 72 A10 "Y/M/D" Date Observation date (UT) from ALMA archive
74- 78 F5.3 arcsec Bmaj [0.02/1.7]? Angular beam size along major
axis (2)
80- 84 F5.3 arcsec Bmin [0.018/1]? Angular beam size along minor axis
(2)
86- 91 F6.2 pc Bmajpc [0.5/670]? Physical beam size along major
axis (2)
93- 98 F6.2 pc Bminpc [0.4/530]? Physical beam size along minor
axis (2)
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Note (1): Calculated from the calibrated data.
Note (2): These are estimated from a reconstructed ALMA image for each target.
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Byte-by-byte Description of file: table3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 2 I2 --- Seq [1/98] Identification number
4 A1 --- f_Seq a: The data of IC 4709 is based on a clean
process with robust=2
6 I1 --- Nspw [0/8] Number of spectral windows (5)
8 I1 --- NwUsed [1/8] Number of spectral windows used for
continuum detections
10- 14 F5.1 GHz Freq [220.8/266.3] Central frequency (6)
16- 20 F5.1 GHz Freqtot [220.8/266.4] Central frequency for entire
data set
22- 24 F3.1 GHz Band [1/7.2] Aggregate bandwidth (7)
26- 28 F3.1 GHz Bandtot [1.9/8] Aggregate bandwidth for entire data
set
30- 35 F6.3 mJy FluxDen [0.05/38] Flux density per beam of peak
emission (8)
37- 41 F5.3 mJy Sigma [0.008/0.2] Noise level; mJy/beam (8)
43- 48 F6.1 --- Signif [2/1147] Detection significance of peak
emission
50- 52 A3 --- UppLim Upper 5sigma limit flag for logF and logL
54- 59 F6.2 [mW/m2] logFlux [-15.7/-13] Log of mm-wave flux; erg/cm2/s
61- 65 F5.2 [10-7W] logLum [36.2/41.1] Log of mm-wave luminosity; erg/s
67- 70 F4.2 [-] Err [0.04/0.1]? Errors in logF and logL (9)
72- 76 F5.2 --- SpInd [-2.5/5]? Spectral index (10)
78- 81 F4.2 --- e_SpInd [0.2/3]? Uncertainty in spectral index
83- 85 A3 --- MFlag Morphology flag (11)
87- 91 F5.2 --- Nansig [1/26]? Number of annuli with significant
non-nuclear emission
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Note (5): Windows where mm-wave emission was significantly detected.
Note (6): Frequency for the collapsed spectral window after removing any
emission line flux.
Note (7): Used for continuum detections.
Note (8): We note that this does not consider systematic uncertainty. We also
note that the quantities in FluxDen and Sigma were derived in
the images after the primary-beam correction.
Note (9): In units of erg/cm2/s for the fluxes and erg/s for the luminosities.
Note (10): Spectral index defined as
Speakν,mm∝ν-αmm.
Note (11): Morphological components were identified in Section 4.
e = extended emission;
b = blob-like emission.
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History:
From electronic version of the journal
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(End) Prepared by [AAS], Emmanuelle Perret [CDS] 29-Jan-2024