J/ApJ/905/57 Herschel/PACS OH doublets sp. of active galaxies (Runco+, 2020)
Herschel/PACS OH spectroscopy of Seyfert, LINER, and starburst galaxies.
Runco J.N., Malkan M.A., Fernandez-Ontiveros J.A., Spinoglio L.,
Pereira-Santaella M.
<Astrophys. J., 905, 57 (2020)>
=2020ApJ...905...57R 2020ApJ...905...57R
ADC_Keywords: Active gal. nuclei; Galaxies, Seyfert; Spectra, infrared;
Equivalent widths
Keywords: Active galaxies ; Seyfert galaxies ; Galaxy counts ;
Infrared galaxies
Abstract:
We investigated the 65, 71, 79, 84, 119, and 163µm OH doublets of
178 local (0<z<0.35) galaxies. They were observed using the
Herschel/Photoconductor Array Camera and Spectrometer, including
Seyfert galaxies, low-ionization nuclear emission-line regions, and
star-forming galaxies. We observe these doublets exclusively in
absorption (OH71), primarily in absorption (OH65, OH84), mostly in
emission (OH79), only in emission (OH163), and an approximately even
mix of the both (OH119). In 19 galaxies we find P Cygni or reverse P
Cygni line profiles in the OH doublets. We use several galaxy
observables to probe spectral classification, brightness of a central
active galactic nucleus (AGN)/starburst component, and radiation field
strength. We find that OH79, OH119, and OH163 are more likely to
display strong emission for bright, unobscured AGNs. For less
luminous, obscured AGNs and nonactive galaxies, we find populations of
strong absorption (OH119), weaker emission (OH163), and a mix of weak
emission and weak absorption (OH79). For OH65, OH71, and OH84, we do
not find significant correlations with the observables listed above.
For OH79 and OH119, we find relationships with both the 9.7µm
silicate feature and Balmer decrement dust extinction tracers in which
more dust leads to weaker emission/stronger absorption. The origin of
emission for the observed OH doublets, whether from collisional
excitation or from radiative pumping by infrared photons, is
discussed.
Description:
A sample of 178 local (z<0.35) galaxies were selected from the
Herschel Science Archive, which were observed with the PACS
instrument. PACS used an integral field spectrograph with a 5x5 square
spaxel detector, which covers a field of view of 47"x47". The spectral
resolution is wavelength dependent, with a range of R=1000-4000
(Δν=75-300km/s). PACS spans a wavelength range of 51-206um.
The observations originated from many different Herschel proposals.
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 86 178 The sample
table3.dat 69 178 IRAS data
table4.dat 69 178 9.7 micron Silicate & Balmer data
table5.dat 107 178 Derived OH integrated flux values
table6.dat 112 178 Derived EW(OH) values
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See also:
II/125 : IRAS catalogue of Point Sources, Version 2.0 (IPAC 1986)
II/156 : IRAS Faint Source Catalog, |b| > 10, Version 2.0 (Moshir+ 1989)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
VII/258 : Quasars and Active Galactic Nuclei (13th Ed.) (Veron+ 2010)
VI/139 : Herschel Observation Log (Herschel Science Centre, 2013)
J/ApJ/453/616 : JHKL photometry of 12 micron galaxy sample (Spinoglio+ 1995)
J/ApJS/112/315 : Spectroscopic parameters of Seyfert nuclei (Ho+ 1997)
J/A+A/417/515 : I Zw 1 unusual emission line spectrum (Veron-Cetty+, 2004)
J/A+A/432/369 : Leiden Atomic & Molecular Database (LAMDA) (Schoeier+, 2005)
J/ApJS/182/628 : Spitzer quasar and ULIRG evolution study (Veilleux+, 2009)
J/ApJS/190/233 : Spectroscopy & abund. of SINGS galaxies (Moustakas+, 2010)
J/ApJ/709/1257 : Spitzer-IRS sp. of Seyfert galaxies. II. (Tommasin+, 2010)
J/MNRAS/414/702 : Optical classification of southern ULIRGs (Lee+, 2011)
J/A+A/578/A74 : Nuclear obscuration in LINERs (Gonzalez-Martin+, 2015)
J/ApJ/803/109 : Spitzer/IRS sp. decompositon of AGN (Hernan-Caballero+, 2015)
J/ApJS/226/19 : FIR sp. of AGNs from Herschel (Fernandez-Ontiveros+, 2016)
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- ID Object identifier
17- 18 I2 h RAh Hour of Right Ascension (J2000) (1)
20- 21 I2 min RAm Minute of Right Ascension (J2000) (1)
23- 29 F7.4 s RAs Second of Right Ascension (J2000) (1)
31- 31 A1 --- DE- Sign of the Declination (J2000) (1)
32- 33 I2 deg DEd Degree of Declination (J2000) (1)
35- 36 I2 arcmin DEm Arcminute of Declination (J2000) (1)
38- 44 F7.4 arcsec DEs Arcsecond of Declination (J2000) (1)
46- 54 F9.7 --- z [0.00067/0.33] Spectroscopic redshift from NED
56- 66 A11 --- Class Optical spectral classification (2)
68- 86 A19 um Trans OH doublet transition(s) observed (3)
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Note (1): From the 2MASS Point Source Catalog (Cat. VII/233).
Note (2): From the Veron-Cetty & Veron (2010, VII/258) catalog.
Note (3): Fine-structure transitions (Table 1):
-------------------------------------------------------------------------------
Line Energy levels Wavelength ΔEul/k Aul
(um) (K) (s-1)
-------------------------------------------------------------------------------
OH65 2Π3/2(J=9/2) 65.132, 65.279 512.1, 510.9 1.276, 1.267
←> 2Π_3/2(J=7/2)
OH71 2Π1/2(J=7/2) 71.171, 71.215 617.6, 617.9 1.014, 1.012
←> 2Π1/2(J=5/2)
OH79 2Π1/2(J=1/2) 79.116, 79.179 181.9, 181.7 0.03606, 0.03598
←> 2Π3/2(J=3/2)
OH84 2Π3/2(J=7/2) 84.420, 84.596 291.2, 290.5 0.5235, 0.5202
←> 2Π3/2(J=5/2)
OH119 2Π3/2(J=5/2) 119.234, 119.441 120.7, 120.5 0.1388, 0.1380
←> 2Π3/2(J=3/2)
OH163 2Π1/2(J=3/2)
←> 2Π1/2(J=1/2) 163.015, 163.396 270.2, 269.8 0.06483, 0.06450
-------------------------------------------------------------------------------
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- ID Object identifier
17- 36 A20 --- Cat IRAS catalog used (4)
38 A1 --- l_F25 Limit flag on F25
39- 45 F7.3 Jy F25 [0.02/274.3]? IRAS 25 micron band flux density
47- 52 F6.3 Jy e_F25 [0.014/11]? Uncertainty in F25
54 A1 --- l_F60 Limit flag on F60
55- 62 F8.3 Jy F60 [0.07/1170]? IRAS 60 micron band flux density
64- 69 F6.3 Jy e_F60 [0.009/59]? Uncertainty in F60
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Note (4): Reference as follows:
PSC v2.1 = IRAS PSC, v2.1. (111 occurrences)
PSC v2.0 = IRAS cat. of Point Sources, v2.0 (Cat. II/125 ;
44 occurrences)
FSC v2.0 = IRAS Faint Source Cat., v2.0 (II/156 ; 11 occurrences)
Golombek et al. 1988 = 1988AJ.....95...26G 1988AJ.....95...26G (4 occurrences)
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 15 A15 --- ID Object identifier
19- 24 F6.3 --- SiStr [-4.1/3.5]? Strength of silicate 9.7um
feature (5)
26- 30 F5.3 --- e_SiStr [0.001/1.1]? Uncertainty in SiStr
32- 36 A5 --- r_SiStr Reference code(s) for SiStr (6)
38- 44 F7.2 10-14mW/m2 Ha [0.09/1385]? Hα line flux;
in 10-14erg/s/cm2 units
46- 51 F6.2 10-14mW/m2 Hb [0.05/503]? Hβ line flux
in 10-14erg/s/cm2 units
53- 69 A17 --- Refs Reference code(s) for line fluxes (7)
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Note (5): Where a negative value indicates an absorption feature, and a
positive value indicates emission (as defined in
Spoon+ 2007ApJ...654L..49S 2007ApJ...654L..49S).
Note (6): Reference code as follows:
ALO16 = Alonso-Herrero et al. (2016MNRAS.455..563A 2016MNRAS.455..563A)
FAR13 = Farrah et al. (2013ApJ...776...38F 2013ApJ...776...38F)
GM15 = Gonzalez-Martin et al. (2015A&A...578A..74G 2015A&A...578A..74G)
HER15 = Hernan-Caballero et al. (2015ApJ...803..109H 2015ApJ...803..109H)
WU09 = Wu et al. (2009ApJ...701..658W 2009ApJ...701..658W)
Note (7): Reference code as follows:
COH81 = Cohen & Osterbrock (1981ApJ...243...81C 1981ApJ...243...81C)
CON12 = Contini (2012MNRAS.426..719C 2012MNRAS.426..719C)
DIA88 = Diaz et al. (1988A&A...195...53D 1988A&A...195...53D)
DUR88 = Durret & Bergeron (1988A&AS...75..273D 1988A&AS...75..273D)
ERK97 = Erkens et al. (1997A&A...323..707E 1997A&A...323..707E)
Reddening corrected values.
GIL10 = Gilli et al. (2010A&A...519A..92G 2010A&A...519A..92G)
GOO83 = Goodrich & Osterbrock (1983ApJ...269..416G 1983ApJ...269..416G)
HO93 = Ho, Filippenko & Sargent (1993ApJ...417...63H 1993ApJ...417...63H)
Observed fluxes.
HO97 = Ho, Filippenko & Sargent (1997ApJS..112..315H 1997ApJS..112..315H)
KOS78 = Koski (1978ApJ...223...56K 1978ApJ...223...56K)
KRA94 = Kraemer et al. (1994ApJ...435..171K 1994ApJ...435..171K)
MAL86 = Malkan (1986ApJ...310..679M 1986ApJ...310..679M) Observed fluxes.
MAL17 = Malkan et al. (2017ApJ...846..102M 2017ApJ...846..102M)
MOR88 = Morris & Ward (1988MNRAS.230..639M 1988MNRAS.230..639M)
MOU10 = Moustakas et al. (2010ApJS..190..233M 2010ApJS..190..233M)
OKE79 = Oke & Lauer (1979ApJ...230..360O 1979ApJ...230..360O)
OST75 = Osterbrock & Miller (1975ApJ...197..535O 1975ApJ...197..535O)
OST81 = Osterbrock (1981ApJ...249..462O 1981ApJ...249..462O)
OST83 = Osterbrock & Dahari (1983ApJ...273..478O 1983ApJ...273..478O)
OST93 = Osterbrock & Martel (1993ApJ...414..552O 1993ApJ...414..552O)
PHI83 = Phillips et al. (1983ApJ...266..485P 1983ApJ...266..485P)
SHU80 = Shuder (1980ApJ...240...32S 1980ApJ...240...32S)
SHU81 = Shuder & Osterbrock (1981ApJ...250...55S 1981ApJ...250...55S)
VAC97 = Vaceli et al. (1997AJ....114.1345V 1997AJ....114.1345V)
VEI95 = Veilleux et al. (1995ApJS...98..171V 1995ApJS...98..171V)
VER04 = Veron-Cetty et al. (2004A&A...417..515V 2004A&A...417..515V)
WIN92 = Winkler (1992MNRAS.257..677W 1992MNRAS.257..677W)
Corrected for Galaxy reddening.
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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- 15 A15 --- ID Object identifier
19 A1 --- l_OH65 Limit flag on OH65
20- 26 F7.2 10-14mW/m2 OH65 [-235/28]? OH65 doublet integrated flux (8)
28- 32 F5.2 10-14mW/m2 e_OH65 [2/29]? Uncertainty in OH65 (9)
34 A1 --- l_OH71 Limit flag on OH71
35- 41 F7.2 10-14mW/m2 OH71 [-446/-4.6]? OH71 doublet integrated flux (8)
43- 46 F4.2 10-14mW/m2 e_OH71 [1.9/7.3]? Uncertainty in OH71 (9)
48 A1 --- l_OH79 Limit flag on OH79
49- 55 F7.2 10-14mW/m2 OH79 [-790/96.1]? OH79 doublet integrated flux (8)
57- 61 F5.2 10-14mW/m2 e_OH79 [0.5/80]? Uncertainty in OH79 (9)
63 A1 --- l_OH84 Limit flag on OH84
64- 70 F7.2 10-14mW/m2 OH84 [-641/33]? OH84 doublet integrated flux (8)
72- 77 F6.2 10-14mW/m2 e_OH84 [0.4/103]? Uncertainty in OH84 (9)
79 A1 --- l_OH119 Limit flag on OH119
80- 87 F8.2 10-14mW/m2 OH119 [-1909/64]? OH119 doublet integrated flux (8)
89- 93 F5.2 10-14mW/m2 e_OH119 [0.14/25]? Uncertainty in OH119 (9)
95 A1 --- l_OH163 Limit flag on OH163
96-101 F6.2 10-14mW/m2 OH163 [-3.8/156]? OH163 doublet integrated flux (8)
103-107 F5.2 10-14mW/m2 e_OH163 [0.27/18.4]? Uncertainty in OH163 (9)
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Note (8): In units of 10-14erg/s/cm2.
Note (9): Note that if an integrated flux measurement does not have an
uncertainty value, it is an upper limit observation. If there is an
uncertainty, it is a detection.
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Byte-by-byte Description of file: table6.dat
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Bytes Format Units Label Explanations
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1- 15 A15 --- ID Object identifier
19- 29 A11 --- Class Optical spectral classification
31 A1 --- l_OH65ew Limit flag on OH65ew
32- 37 F6.3 um OH65ew [-0.03/0.2]? OH65 doublet equivalent width (10)
39- 43 F5.3 um e_OH65ew [0]? Uncertainty in OH65ew (11)
44 A1 --- l_OH71ew Limit flag on OH71ew
45- 50 F6.3 um OH71ew [-0.02/0.02]? OH71 doublet equivalent width (10)
52- 56 F5.3 um e_OH71ew [0.001/0.004]? Uncertainty in OH71ew (11)
58 A1 --- l_OH79ew Limit flag on OH79ew
59- 64 F6.3 um OH79ew [-0.03/0.64]? OH79 doublet equivalent width (10)
66- 70 F5.3 um e_OH79ew [0.001/0.12]? Uncertainty in OH79ew (11)
72 A1 --- l_OH84ew Limit flag on OH84ew
73- 78 F6.3 um OH84ew [-0.06/0.05]? OH84 doublet equivalent width (10)
80- 84 F5.3 um e_OH84ew [0.001/0.02]? Uncertainty in OH84ew (11)
86 A1 --- l_OH119ew Limit flag on OH119ew
87- 92 F6.3 um OH119ew [-0.17/0.4]? OH119 doublet equivalent width (10)
94- 98 F5.3 um e_OH119ew [0.001/0.06]? Uncertainty in OH119ew (11)
100 A1 --- l_OH163ew Limit flag on OH163ew
101-106 F6.3 um OH163ew [0.008/0.2]? OH163 doublet equivalent width (10)
108-112 F5.3 um e_OH163ew [0.002/0.04]? Uncertainty in OH163ew (11)
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Note (10): Where a negative value indicates an absorption feature, and a
positive value indicates emission.
Note (11): Note that if an equivalent width measurement does not have an
uncertainty value, it is an upper limit observation. If there is an
uncertainty, it is a detection.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 16-May-2022