J/A+A/691/A203 Multiwavelength properties of unobscured AGN (Gupta+, 2024)
BASS. XLIII. Optical, UV, and X-ray emission properties of unobscured Swift/BAT
active galactic nuclei.
Gupta K.K., Ricci C., Temple M.J., Tortosa A., Koss M.J., Assef R.J.,
Bauer F.E., Mushotzy R., Ricci F., Ueda Y., Rojas A.F., Trakhtenbrot B.,
Chang C.-S., Oh K., Li R., Kawamuro T., Diaz Y., Powell M.C., Stern D.,
Urry C.M., Harrison F., Cenko B.
<Astron. Astrophys. 691, A203 (2024)>
=2024A&A...691A.203G 2024A&A...691A.203G (SIMBAD/NED BibCode)
ADC_Keywords: Active gal. nuclei ; Galaxies, Seyfert ; Photometry ;
Spectroscopy ; Optical ; X-ray sources ; Ultraviolet
Keywords: galaxies: active - galaxies: Seyfert - quasars: general -
quasars: supermassive black holes
Abstract:
We present one of the largest multiwavelength studies of simultaneous
optical-to-X-ray spectral energy distributions (SEDs) of unobscured
(N_H<1022cm-2) active galactic nuclei (AGN) in the local Universe.
Using a representative sample of hard-X-ray-selected AGN from the
70-month Swift/BAT catalog, with optical/UV photometric data from
Swift/UVOT and X-ray spectral data from Swift/XRT, we constructed
broadband SEDs of 236 nearby AGN (0.001<z<0.3). We employed GALFIT to
estimate host galaxy with a reflection component to model the X-ray
spectra and a dust-reddened multi-temperature blackbody to fit the
optical/UV SED. We calculated intrinsic luminosities at multiple
wavelengths, total bolometric luminosities (Lbol), optical-to-X-ray
spectral indices (αox), and multiple bolometric corrections
(κλ) in the optical, UV, and X-rays. We used black hole
masses obtained by reverberation mapping and the virial method to
estimate Eddington ratios (λEdd) for all our AGN. We confirm
the tight correlation (scatter=0.45dex) between UV (2500Å) and
X-ray (2keV) luminosity for our sample. We observe a significant
decrease in αox with Lbol and λEdd, suggesting that
brighter sources emit more UV photons per X-rays. We report a
second-order regression relation (scatter=0.15dex) between the 2-10keV
bolometric correction (κ2-10) and αox, which is useful
to compute Lbol in the absence of multiband SEDs. We also investigate
the dependence of optical/UV bolometric corrections on the physical
properties of AGN and obtain a significant increase in the UV
bolometric corrections (κW2 and κM2) with Lbol and
λEdd, unlike those in the optical (κV and
κB), which are constant across five orders of L_bol and
λEdd. We obtain significant dispersions (∼0.1-1dex) in all
bolometric corrections, and hence recommend using appropriate
relations with observed quantities while including the reported
scatter, instead of their median values.
Description:
In this paper, we present one of the largest studies to date of
optical-to-X-ray wavelength SEDs for a sample of 236 unobscured,
hard-X-ray-selected, nearby AGN from the 70-month Swift/BAT catalog.
We compiled simultaneous optical, UV, and X-ray observations for all
sources to mitigate any issues arising due to differences in the
variability timescales at different wavelengths. We extracted the
0.3-10keV X-ray spectra and magnitudes and fluxes in the six
Swift/UVOT filters: V, B, U, UVW1, UVM2, and UVW2 for all our sources.
We corrected the optical/ UV fluxes for galactic dust extinction as
well as host galaxy contamination. The latter was done by fitting the
2D surface brightness of the source images using a PSF and a Sersic
profile with GALFIT to fit the AGN and the host galaxy, respectively.
We also performed numerous simulations by creating fake populations of
type I AGN and fitting them using GALFIT, to quantitatively inspect
the reliability of the AGN magnitudes calculated by GALFIT. As a
result of these simulations, we were able to calculate correction
factors in each of the six Swift/UVOT filters, which can be used to
correct the GALFIT-estimated PSF fluxes. We constructed and fit the
multiwavelength AGN SEDs (10-7 to 500keV) using a dust-reddened
multi-temperature blackbody to model the optical/UV accretion disk and
a variety of X-ray models consisting of multiple components to account
for the primary X-ray emission and the reprocessed secondary emission.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tablea1.dat 91 293 *For all the 293 unobscured AGN sources in our
sample, with simultaneous optical/UV
and X-ray observations
tablea2.dat 61 293 *For all the 293 unobscured AGN sources in our
sample, with simultaneous optical/UV and
X-ray observations
tablea3.dat 90 292 *For all the 292 unobscured AGN sources in our
sample, with optical/UV photometry
tablea4.dat 90 292 *For all the 292 unobscured AGN sources in our
sample, with optical/UV photometry
tablea5.dat 82 290 *For all the 290 unobscured AGN sources in our
sample, with X-ray spectroscopy
tablea6.dat 104 236 *For all the 236 unobscured AGN sources in our
final SED sample
tablea7.dat 110 236 *For all the 236 unobscured AGN sources in our
final SED sample
tablea8.dat 85 236 *For all the 236 unobscured AGN sources in our
final SED sample
tablea9.dat 109 236 *For all the 236 unobscured AGN sources in our
final SED sample
tablea10.dat 68 236 *For all the 236 unobscured AGN sources in our
final SED sample
--------------------------------------------------------------------------------
Note on tablea1.dat: we have listed their BAT and Swift IDs, counterpart names,
coordinates, redshifts, luminosity distances, and X-ray column density values.
Note on tablea2.dat: we have listed their observation IDs, and for each
observation we have listed the total UVOT and XRT exposures, and the available
Swift/UVOT filters.
Note on tablea3.dat: we have listed the source fluxes calculated using the
Swift/UVOT command 'uvotsource' via 5σ aperture photometry,
in all available bands.
Note on tablea4.dat: we have listed the source magnitudes calculated using the
Swift/UVOT command 'uvotsource' via 5σ aperture photometry,
in all available bands.
Note on tablea5.dat: we have listed the final outputs of the spectral fitting,
including the best-fit values of the photon index, the 2-10keV intrinsic
fluxes, the model used to get the best fit, and the value of the cash
statistic and the degrees of freedom of the fit.
Note on tablea6.dat: we have listed the corrected AGN fluxes estimated by
GALFIT image decomposition, in all available bands.
Note on tablea7.dat: we have listed the corrected AGN magnitudes estimated by
GALFIT image decomposition, in all available bands.
Note on tablea8.dat: we have listed the final outputs of the optical/UV SED
fitting, including the best-fit values of the disk temperature, the
extinction due to the host galaxy, and the total intrinsic optical/UV flux.
Note on tablea9.dat: we have listed their 2500Å, 2keV, and bolometric
luminosities. We have also reported their black hole masses, optical-to-X-ray
spectral indices, 2-10keV X-ray bolometric corrections, the 4400Å optical
bolometric corrections, and Eddington ratios.
Note on tablea10.dat: we have listed their optical/UV bolometric corrections
in the six Swift/UVOT bands.
--------------------------------------------------------------------------------
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)
J/ApJS/269/24 : BASS. XXXIV. ALMA obs. of Swift/BAT AGNs (Kawamuro+, 2023)
Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 50 A25 --- Ctp Name of the source counterpart
52- 59 F8.4 deg RAdeg Right ascension of the source (J2000.0)
61- 68 F8.4 deg DEdeg Declination of the source (J2000.0)
70- 75 F6.4 --- z Redshift of the source
77- 82 F6.1 Mpc Dist Luminosity distance of the source (1)
84- 88 F5.2 [cm-2] log(NH) ?=- Log of the X-ray column density of the
source (2)
90- 91 A2 --- l_log(NH) [UL -] Upper limit flag on the X-ray
column density (3)
--------------------------------------------------------------------------------
Note (1): From Koss et al. (2022ApJS..261....2K 2022ApJS..261....2K, Cat. J/ApJS/261/2).
Note (2): From Ricci et al. (2017ApJS..233...17R 2017ApJS..233...17R, Cat. J/ApJS/233/17).
Note (3): 'UL', when the X-ray column density is an upper limit.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 35 A10 --- ObsID Observation ID for the source
37- 41 I5 s UVOT-Texp Total Swift/UVOT exposure time
43- 47 I5 s XRT-Texp Total Swift/XRT exposure time
49- 61 A13 --- Filters All available Swift/UVOT filters
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 30 F5.2 10-18W/m2 FU ?=- Source flux in the Swift/UVOT U band (1)
32- 35 F4.2 10-18W/m2 e_FU ?=- Error on the source flux in the
Swift/UVOT U band (1)
37- 41 F5.2 10-18W/m2 FV ?=- Source flux in the Swift/UVOT V band (1)
43- 46 F4.2 10-18W/m2 e_FV ?=- Error on the source flux in the
Swift/UVOT V band (1)
48- 52 F5.2 10-18W/m2 FB ?=- Source flux in the Swift/UVOT B band (1)
54- 57 F4.2 10-18W/m2 e_FB ?=- Error on the source flux in the
Swift/UVOT B band (1)
59- 63 F5.2 10-18W/m2 FUVW1 ?=- Source flux in the Swift/UVOT UVW1 band (1)
65- 68 F4.2 10-18W/m2 e_FUVW1 ?=- Error on the source flux in the
Swift/UVOT UVW1 band (1)
70- 74 F5.2 10-18W/m2 FUVW2 ?=- Source flux in the Swift/UVOT UVW2 band (1)
76- 79 F4.2 10-18W/m2 e_FUVW2 ?=- Error on the source flux in the
Swift/UVOT UVW2 band (1)
81- 85 F5.2 10-18W/m2 FUVM2 ?=- Source flux in the Swift/UVOT UVM2 band (1)
87- 90 F4.2 10-18W/m2 e_FUVM2 ?=- Error on the source flux in the
Swift/UVOT UVM2 band (1)
--------------------------------------------------------------------------------
Note (1): In 10-15erg/cm2/s/Å.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 30 F5.2 mag Vmag ?=- Source magnitude in the
Swift/UVOT V band (AB)
32- 35 F4.2 mag e_Vmag ?=- Error on the source magnitude in the
Swift/UVOT V band (AB)
37- 41 F5.2 mag Bmag ?=- Source magnitude in the
Swift/UVOT B band (AB)
43- 46 F4.2 mag e_Bmag ?=- Error on the source magnitude in the
Swift/UVOT B band (AB)
48- 52 F5.2 mag Umag ?=- Source magnitude in the
Swift/UVOT U band (AB)
54- 57 F4.2 mag e_Umag ?=- Error on the source magnitude in the
Swift/UVOT U band (AB)
59- 63 F5.2 mag UVW1mag ?=- Source magnitude in the
Swift/UVOT UVW1 band (AB)
65- 68 F4.2 mag e_UVW1mag ?=- Error on the source magnitude in the
Swift/UVOT UVW1 band (AB)
70- 74 F5.2 mag UVM2mag ?=- Source magnitude in the
Swift/UVOT UVM2 band (AB)
76- 79 F4.2 mag e_UVM2mag ?=- Error on the source magnitude in the
Swift/UVOT UVM2 band (AB)
81- 85 F5.2 mag UVW2mag ?=- Source magnitude in the
Swift/UVOT UVW2 band (AB)
87- 90 F4.2 mag e_UVW2mag ?=- Error on the source magnitude in the
Swift/UVOT UVW2 band (AB)
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea5.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 29 F4.2 --- Gamma Photon index of the X-ray power law
31- 34 F4.2 --- e_Gamma ?=- Lower error on the photon index
36- 40 F5.2 --- E_Gamma ?=- Upper error on the photon index
42- 46 F5.2 10-15W/m2 F(2-10) Flux in the 2-10 keV energy range (1)
48- 51 F4.2 10-15W/m2 e_F(2-10) Lower error on the 2-10 keV flux (1)
53- 56 F4.2 10-15W/m2 E_F(2-10) Upper error on the 2-10 keV flux (1)
58- 68 A11 --- Model Best-fit X-ray model
70- 76 F7.2 --- Statistic C-statistic of the best fit
78- 82 F5.1 --- Dof Degrees of freedom
--------------------------------------------------------------------------------
Note (1): In 10-12erg/cm2/s.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea6.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 30 F5.2 10-17W/m2/nm FV ?=- AGN flux in the Swift/UVOT V band (1)
32- 35 F4.2 10-17W/m2/nm e_FV ?=- Error on the AGN flux in the
Swift/UVOT V band (1)
37 A1 --- f_FV [op-] Flag for the AGN flux in the
Swift/UVOT V band (2)
39- 43 F5.2 10-17W/m2/nm FB ?=- AGN flux in the Swift/UVOT B band (1)
45- 48 F4.2 10-17W/m2/nm e_FB ?=- Error on the AGN flux in the
Swift/UVOT B band (1)
50 A1 --- f_FB [op-] Flag for the AGN flux in the
Swift/UVOT B band (2)
52- 56 F5.2 10-17W/m2/nm FU ?=- AGN flux in the Swift/UVOT U band (1)
58- 61 F4.2 10-17W/m2/nm e_FU ?=- Error on the AGN flux in the
Swift/UVOT U band (1)
63 A1 --- f_FU [op-] Flag for the AGN flux in the
Swift/UVOT U band (2)
65- 69 F5.2 10-17W/m2/nm FUVW1 AGN flux in the Swift/UVOT UVW1 band (1)
71- 74 F4.2 10-17W/m2/nm e_FUVW1 Error on the AGN flux in the
Swift/UVOT UVW1 band (1)
76 A1 --- f_FUVW1 [op-] Flag for the AGN flux in the
Swift/UVOT UVW1 band (2)
78- 82 F5.2 10-17W/m2/nm FUVM2 ?=- AGN flux in the Swift/UVOT UVM2 band (1)
84- 87 F4.2 10-17W/m2/nm e_FUVM2 ?=- Error on the AGN flux in the
Swift/UVOT UVM2 band (1)
89 A1 --- f_FUVM2 [op-] Flag for the AGN flux in the
Swift/UVOT UVM2 band (2)
91- 95 F5.2 10-17W/m2/nm FUVW2 ?=- AGN flux in the Swift/UVOT UVW2 band (1)
97-100 F4.2 10-17W/m2/nm e_FUVW2 ?=- Error on the AGN flux in the
Swift/UVOT UVW2 band (1)
102 A1 --- f_FUVW2 [op-] Flag for the AGN flux in the
Swift/UVOT UVW2 band (2)
104 A1 --- Flag [c-] Flag for the final
GALFIT-estimated fluxes (3)
--------------------------------------------------------------------------------
Note (1): In 10-15erg/cm2/s/Å.
Note (2): Flag as follows:
o = if a sky + PSF model was used to get the best GALFIT residual when
GALFIT was unable to fit a Sersic profile
p = if Swift/UVOT pipeline-estimated flux was used in the final SED
Note (3): Flag as follows:
c = if the GALFIT-estimated AGN fluxes were corrected, using corrections
calculated in Sect. 5.3, to create the final SEDs
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea7.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 30 F5.2 mag Vmag ?=- AGN magnitude in the Swift/UVOT V band (AB)
32- 36 F5.3 mag e_Vmag ?=- Error on the AGN magnitude in the
Swift/UVOT V band (AB)
38 A1 --- f_Vmag [op-] Flag for the AGN magnitude in the
Swift/UVOT V band (1)
40- 44 F5.2 mag Bmag ?=- AGN magnitude in the Swift/UVOT B band (AB)
46- 51 F6.4 mag e_Bmag ?=- Error on the AGN magnitude in the
Swift/UVOT B band (AB)
53 A1 --- f_Bmag [op-] Flag for the AGN magnitude in the
Swift/UVOT B band (1)
55- 59 F5.2 mag Umag ?=- AGN magnitude in the Swift/UVOT U band (AB)
61- 64 F4.2 mag e_Umag ?=- Error on the AGN magnitude in the
Swift/UVOT U band (AB)
66 A1 --- f_Umag [op-] Flag for the AGN magnitude in the
Swift/UVOT U band (1)
68- 72 F5.2 --- UVW1mag AGN magnitude in the Swift/UVOT UVW1 band (AB)
74- 78 F5.3 --- e_UVW1mag Error on the AGN magnitude in the
Swift/UVOT UVW1 band (AB)
80 A1 --- f_UVW1mag [op-] Flag for the AGN magnitude in the
Swift/UVOT UVW1 band (1)
82- 86 F5.2 mag UVM2mag ?=- AGN magnitude in the
Swift/UVOT UVM2 band (AB)
88- 93 F6.4 mag e_UVM2mag ?=- Error on the AGN magnitude in the
Swift/UVOT UVM2 band (AB)
95 A1 --- f_UVM2mag [op-] Flag for the AGN magnitude in the
Swift/UVOT UVM2 band (1)
97-101 F5.2 mag UVW2mag ?=- AGN magnitude in the
Swift/UVOT UVW2 band (AB)
103-106 F4.2 mag e_UVW2mag ?=- Error on the AGN magnitude in the
Swift/UVOT UVW2 band (AB)
108 A1 --- f_UVW2mag [op-] Flag for the AGN magnitude in the
Swift/UVOT UVW2 band (1)
110 A1 --- Flag [c-] Flag for the final GALFIT-estimated
magnitudes (2)
--------------------------------------------------------------------------------
Note (1): Flag as follows:
o = if a sky + PSF model was used to get the best GALFIT residual when
GALFIT was unable to fit a Sersic profile
p = if Swift/UVOT pipeline-estimated magnitude was used in the final SED
Note (2): Flag as follows:
c = if the GALFIT-estimated AGN magnitudes were corrected, using corrections
calculated in Sect. 5.3, to create the final SEDs
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea8.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 29 F4.1 eV kTmax Maximum disk temperature
31- 35 F5.2 eV e_kTmax ?=- Lower error on the
maximum disk temperature
37- 41 F5.2 eV E_kTmax ?=- Upper error on the
maximum disk temperature
43- 47 F5.3 --- E(B-V)HG Dust extinction due to host galaxy
49- 53 F5.3 --- e_E(B-V)HG ?=- Lower error on the dust extinction
due to host galaxy
55- 59 F5.3 --- E_E(B-V)HG ?=- Upper error on the dust extinction
due to host galaxy
61- 62 A2 --- l_E(B-V)HG [UL -] Upper limit flag for the host galaxy
dust extinction (1)
64- 69 F6.2 10-14W/m2 Fuvo Flux in the 10-7 to 0.1keV optical/UV
energy range (2)
71- 75 F5.2 10-14W/m2 e_Fuvo Lower error on the flux in the 10-7
to 0.1keV optical/UV energy range (2)
77- 82 F6.2 10-14W/m2 E_Fuvo Upper error on the flux in the 10-7
to 0.1keV optical/UV energy range (2)
84- 85 A2 --- Flag [te- ] Flag for the SED fitting
procedure (3)
--------------------------------------------------------------------------------
Note (1): 'UL', if the host galaxy dust extinction is an upper limit.
Note (2): In 10-11erg/cm2/s
Note (3): Flag as follows:
t = if the maximum disk temperature was fixed to its median value of 2.7 eV
e = if the host galaxy dust extinction was fixed to zero
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea9.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 30 F5.2 [10-7W] L2500 Log of the intrinsic,
monochromatic luminosity at 2500Å
32- 36 F5.2 [10-7W] L2keV Log of the intrinsic,
monochromatic luminosity at 2keV
38- 42 F5.2 [10-7W] Lbol Log of the bolometric luminosity
44- 47 F4.2 Msun MBH ? Log of the black hole mass (1)
49- 53 F5.2 --- alphaox Optical-to-X-ray spectral index
55- 58 F4.2 --- e_alphaox Lower error on the optical-to-X-ray
spectral index
60- 64 F5.2 --- E_alphaox Upper error on the optical-to-X-ray
spectral index
66- 70 F5.2 --- k4400 Bolometric correction at 4400Å
72- 76 F5.2 --- e_k4400 Lower error on the bolometric correction
at 4400Å
78- 83 F6.2 --- E_k4400 Upper error on the bolometric correction
at 4400Å
85- 90 F6.2 --- k(2-10) Bolometric correction in 2-10keV energy range
92- 96 F5.2 --- e_k(2-10) Lower error on the bolometric correction in
2-10keV energy range
98-103 F6.2 --- E_k(2-10) Upper error on the bolometric correction in
2-10keV energy range
105-109 F5.2 [-] ER ? Log of Eddington ratio
--------------------------------------------------------------------------------
Note (1): From Mejia-Restrepo et al. (2022ApJS..261....5M 2022ApJS..261....5M, Cat. J/ApJS/261/5).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea10.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 4 I4 --- BAT BAT ID of the source
6- 24 A19 --- Swift Swift ID of the source
26- 31 F6.2 --- kV Bolometric correction in the Swift/UVOT V band
33- 38 F6.2 --- kB Bolometric correction in the Swift/UVOT B band
40- 45 F6.2 --- kU Bolometric correction in the Swift/UVOT U band
47- 52 F6.2 --- kUVW1 Bolometric correction in the Swift/UVOT UVW1 band
54- 60 F7.2 --- kUVM2 Bolometric correction in the Swift/UVOT UVM2 band
62- 68 F7.2 --- kUVW2 Bolometric correction in the Swift/UVOT UVW2 band
--------------------------------------------------------------------------------
Acknowledgements:
Kriti Kamal Gupta, kkgupta(at)uliege.be
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Kawamuro et al. Paper XXXII. 2022ApJ...938...87K 2022ApJ...938...87K
Marcotulli et al. Paper XXXIII. 2022ApJ...940...77M 2022ApJ...940...77M Cat. J/ApJ/940/77
Kawamuro et al. Paper XXXIV. 2023ApJS..269...24K 2023ApJS..269...24K Cat. J/ApJS/269/24
Caglar et al. Paper XXXV. 2023ApJ...956...60C 2023ApJ...956...60C
Powell et al. Paper XXXVI. 2022ApJ...938...77P 2022ApJ...938...77P
Ricci et al. Paper XXXVII. 2022ApJ...938...67R 2022ApJ...938...67R
Ananna et al. Paper XXXVIII. 2022ApJ...939L..13A 2022ApJ...939L..13A
Temple et al. Paper XXXIX. 2023MNRAS.518.2938T 2023MNRAS.518.2938T
Tortosa et al. Paper XL. 2023MNRAS.526.1687T 2023MNRAS.526.1687T
Ricci et al. Paper XLII. 2023ApJ...959...27R 2023ApJ...959...27R
(End) Kriti Kamal Gupta [UDP, Chile], Patricia Vannier [CDS] 15-Oct-2024