J/ApJS/255/10 WISE MIR variability in gamma-ray Seyfert 1 gal. (Mao+, 2021)
A search for rapid mid-infrared variability in gamma-ray-emitting narrow-line
Seyfert 1 galaxies.
Mao L., Yi T.
<Astrophys. J. Suppl. Ser., 255, 10-10 (2021)>
=2021ApJS..255...10M 2021ApJS..255...10M (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, Seyfert; Photometry, infrared; Redshifts; Gamma rays
Keywords: Seyfert galaxies; Infrared Astronomical Satellite; Infrared photometry
Gamma-ray sources
Abstract:
Fermi-LAT's detection of γ-rays from narrow-line Seyfert 1
galaxies (NLS1s) has received increasing attention. Understanding
these γ-NLS1s is of interest because they have some properties
similar to blazars, which are known to show rapid and large-amplitude
variability. Based on the largest sample of γ-NLS1s (25
sources), we carried out a systematic search for rapid mid-infrared
(MIR, 3.4 and 4.6µm) variability using the multiepoch data of the
Wide-field Infrared Survey Explorer (WISE). We also compared a few
variability properties between γ-NLS1s and γ-ray blazars.
Our main results are as follows. (1) Thirteen γ-NLS1s showed
significant (>3σ) rapid variability in at least one of the two
MIR bands. The MIR emission of these sources is dominated by the
synchrotron emission of relativistic electrons in the jet. (2) The
γ-NLS1s with flat radio spectra are more variable than those not
detected in γ-rays. (3) The γ-NLS1s tend to show smaller
amplitude of variability as well as lower duty cycle relative to
γ-ray blazars. (4) The γ-NLS1s tend to show a trend of
bluer-when-brighter on both intraday and long timescales, similar to
γ-ray blazars. (5) The γ-NLS1s that are more variable on
long timescales have larger amplitudes of variability and higher duty
cycles on intraday timescales. (6) In the majority of cases, the
γ-NLS1s fall in the WISE Gamma-ray Blazar Strip (WGS). However,
we noted migrations outside of the WGS due to significant variability.
Description:
Using the multiepoch data from the first 10 years of observations
(2010-2019) of WISE/NEOWISE, we have carried out a systematic search
for rapid MIR variability (or IDV) in the 3.4 and 4.6um bands for
22 known γ-narrow-line Seyfert 1 and 3 high-confidence candidates.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 105 25 Properties of 25 γ-NLS1s
table2.dat 98 25 ALLWISE data on the sample of γ-NLS1s
table3.dat 92 5073 WISE multi-epoch data of 25 γ-NLS1s
table4.dat 58 368 Variability analysis results of 25 γ-NLS1s
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See also:
II/311 : WISE All-Sky Data Release (Cutri+ 2012)
II/328 : AllWISE Data Release (Cutri+ 2013)
J/ApJS/166/128 : Narrow line Seyfert 1 galaxies from SDSS-DR3 (Zhou+, 2006)
J/ApJS/166/470 : SDSS-Spitzer type I QSOs IR photometry (Richards+, 2006)
J/A+A/487/475 : X-ray variability of AGNs in Lockman Hole (Papadakis+, 2008)
J/ApJ/716/530 : Mid-IR variability from the SDWFS (Kozlowski+, 2010)
J/ApJS/194/29 : Observations of blazars at 15GHz (Richards+, 2011)
J/ApJ/748/68 : WISE IR colors of gamma-ray blazars (D'Abrusco+, 2012)
J/ApJ/748/124 : AGN X-ray variability in the 4Ms catalog (Young+, 2012)
J/MNRAS/438/3058 : 15GHz variability of γ-ray blazars (Richards+, 2014)
J/MNRAS/439/690 : Optical/γ-ray variability in blazars (Hovatta+, 2014)
J/ApJ/792/30 : NEOWISE magnitudes for near-Earth objects (Mainzer+, 2014)
J/ApJ/795/58 : 1H 0323+342 rest frame opt. spectrum with GHAO (Leon+, 2014)
J/A+A/573/A76 : Multifrequency study of NL Seyfert 1 galaxies (Jarvela+, 2015)
J/ApJ/810/14 : Third catalog of LAT-detected AGNs (3LAC) (Ackermann+, 2015)
J/ApJ/817/119 : Spitzer variability survey of Bootes field (Kozlowski+, 2016)
J/ApJS/224/26 : SEDs of Roma BZCAT blazars (Mao+, 2016)
J/AJ/152/12 : MOJAVE. XIII. New 15GHz obs. on 1994-2013 (Lister+, 2016)
J/ApJS/229/39 : Narrow line Seyfert 1 galaxies from SDSS-DR12 (Rakshit+, 2017)
J/A+A/614/L1 : NLS1 at 37GHz (Lahteenmaki+, 2018)
J/A+A/615/A167 : Catalog of NLS1s galaxies in 6dFGS survey (Chen+, 2018)
J/ApJ/881/L24 : Black hole masses of SDSS Seyfert 1 gal. (Viswanath+, 2019)
J/ApJS/247/33 : The Fermi LAT fourth source catalog (4FGL) (Abdollahi+, 2020)
J/ApJ/892/105 : 4th catalog of Fermi LAT-detected AGNs (4LAC) (Ajello+, 2020)
http://wise2.ipac.caltech.edu/docs/release/neowise/
neowise2020release_intro.html : NEOWISE 2020 data release
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 2 I2 --- Seq [1/25] Running sequence number
4- 27 A24 --- Name Name of the γ-narrow-line Seyfert 1
29 A1 --- f_Name d=high-confidence γ-NLS1 candidate
31- 37 F7.3 deg RAdeg [7.99/319.73] Right ascension (J2000)
39- 45 F7.3 deg DEdeg [-44.6/53.2] Declination (J2000)
47- 51 F5.3 --- z [0.061/1.004] Redshift from NED
53 A1 --- Sp Shape of radio spectrum (1)
55 I1 --- r_Sp ? Reference on Sp (2)
57- 60 I4 --- R [11/8140]? Radio-loudness estimation
62 A1 --- r_R Reference on R (2)
64- 67 F4.2 [Msun] logMbh [6.7/8.3] Logarithmic of black hole mass
69- 70 I2 --- r_logMbh [1/29] Reference on logMbh (2)
72- 74 A3 --- Var Variability analysis result from this work (3)
76- 78 A3 --- VJ12 Variability result in MIR band from J12
(Jiang+ 2012ApJ...759L..31J 2012ApJ...759L..31J) (3)
80- 82 A3 --- VGMF18 Variability result from GMF18
(Gabanyi+ 2018rnls.confE..42G) (3)
84- 85 A2 --- Vother Variability result from other previous works
87- 88 I2 --- r_Vother [3/23]? Reference on Vother (2)
90 A1 --- Rad Variability result in radio band
92 A1 --- Opt Variability result optical band
94- 95 I2 --- r_Opt [14/20]? Reference on Opt (2)
97 A1 --- UV Variability result in UV band
99- 100 I2 --- r_UV [20/23]? Reference on UV (2)
102 A1 --- GeV Variability result in GeV band
104- 105 I2 --- r_GeV [24/28]? Reference on GeV (2)
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Note (1): We have used the previous literature and the estimated radio spectral
indices α derived from NED photometric data to classify our
selected γ-NLS1s into flat-spectrum ("F"; α>-0.5) or
steep-spectrum ("S"; α≤-0.5) ones.
Note (2): Reference as follows:
1 = Foschini et al. (2015A&A...575A..13F 2015A&A...575A..13F)
2 = Paliya et al. (2018ApJ...853L...2P 2018ApJ...853L...2P)
3 = Yao et al. (2015MNRAS.454L..16Y 2015MNRAS.454L..16Y)
4 = Gu et al. (2015ApJS..221....3G 2015ApJS..221....3G)
5 = Berton et al. (2017FrASS...4....8B 2017FrASS...4....8B)
6 = Yuan et al. (2008ApJ...685..801Y 2008ApJ...685..801Y)
7 = Komossa (2018rnls.confE..15K)
8 = Jarvela et al. (2015A&A...573A..76J 2015A&A...573A..76J)
9 = Yao et al. (2019MNRAS.487L..40Y 2019MNRAS.487L..40Y)
10 = Rakshit et al. (2017, J/ApJS/229/39)
11 = Zhou et al. (2007ApJ...658L..13Z 2007ApJ...658L..13Z)
12 = Lahteenmaki et al. (2018A&A...614L...1L 2018A&A...614L...1L)
13 = Oshlack et al. (2001ApJ...558..578O 2001ApJ...558..578O)
14 = Paliya et al. (2013MNRAS.428.2450P 2013MNRAS.428.2450P)
15 = Paliya et al. (2016ApJ...819..121P 2016ApJ...819..121P)
16 = Ojha et al. (2021MNRAS.501.4110O 2021MNRAS.501.4110O)
17 = Ojha et al. (2020MNRAS.493.3642O 2020MNRAS.493.3642O)
18 = Ojha et al. (2019MNRAS.483.3036O 2019MNRAS.483.3036O)
19 = Bhattacharya et al. (2019MNRAS.483.3382B 2019MNRAS.483.3382B)
20 = D'Ammando (2020MNRAS.498..859D 2020MNRAS.498..859D)
21 = D'Ammando (2020MNRAS.496.2213D 2020MNRAS.496.2213D)
22 = Bruhweiler et al. (1986ApJ...303L..31B 1986ApJ...303L..31B)
23 = Yang et al. (2018MNRAS.477.5127Y 2018MNRAS.477.5127Y)
24 = Paliya et al. (2014ApJ...789..143P 2014ApJ...789..143P)
25 = D'Ammando et al. (2012MNRAS.426..317D 2012MNRAS.426..317D)
26 = Foschini et al. (2011MNRAS.413.1671F 2011MNRAS.413.1671F)
27 = D'Ammando et al. (2016MNRAS.463.4469D 2016MNRAS.463.4469D)
28 = Gokus et al. (2021A&A...649A..77G 2021A&A...649A..77G)
29 = Paiano et al. (2019ApJ...871..162P 2019ApJ...871..162P)
* = Radio loudness calculated using the NED data
Note (3): Code as follows:
RV = detection of rapid MIR variability
NRV = non-detection of rapid MIR variability
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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- 2 I2 --- Seq [1/25] Running sequence number
4- 27 A24 --- Name Name of the γ-narrow-line Seyfert 1
29- 47 A19 --- WISEA AllWISE counterpart name
49- 54 F6.3 mag W1mag [10.74/14.83] WISE W1 (3.4um) band magnitude
56- 60 F5.3 mag e_W1mag [0.02/0.04] Uncertainty on the W1mag
62- 67 F6.3 mag W2mag [9.79/13.83] WISE W2 (4.6um) band magnitude
69- 73 F5.3 mag e_W2mag [0.02/0.04] Uncertainty on the W2mag
75- 80 F6.3 mag W3mag [7.17/10.9] WISE W3 (12um) band magnitude
82- 86 F5.3 mag e_W3mag [0.016/0.2] Uncertainty on the W3mag
88- 92 F5.3 mag W4mag [4.84/8.45] WISE W4 (22um) band magnitude
94- 98 F5.3 mag e_W4mag [0.027/0.4] Uncertainty on the W4mag
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 24 A24 --- Name Name of the γ-narrow-line Seyfert 1
28- 38 F11.5 d MJD [55204.3/58830.3] Modified Julian Date;
JD-2400000.5
40- 45 F6.3 mag W1mag [10.51/15.3] WISE W1 band magnitude
47- 51 F5.3 mag e_W1mag [0.015/0.2] Uncertainty in W1mag
53- 58 F6.3 mag W2mag [9.56/14.27] WISE W2 band magnitude
60- 64 F5.3 mag e_W2mag [0.013/0.2] Uncertainty in W2mag
66- 69 F4.1 --- SNR1 [7.1/73.5] W1 profile-fit measurement
signal-to-noise ratio
71- 78 E8.2 --- w1rchi2 [0.2/10] Reduced chi-square of the W1
profile-fit photometry measurement
80- 83 F4.1 --- SNR2 [5.4/80.5] W2 profile-fit measurement
signal-to-noise ratio
85- 92 E8.2 --- w2rchi2 [0.18/6.1] Reduced chi-square of the W2
profile-fit photometry measurement
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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- 24 A24 --- Name Name of the γ-narrow-line Seyfert 1
26- 27 I2 --- Nep [1/17] Serial number of observational epoch
29 A1 --- l_V3.4 Limit flag on V3.4
30- 34 F5.1 --- V3.4 [0/100] WISE 3.4um variability index
36 A1 --- l_V4.6 Limit flag on V4.6
37- 41 F5.1 --- V4.6 [0/100] WISE 4.6um variability index
43 A1 --- l_delta3.4 Limit flag for delta3.4
44 I1 --- delta3.4 [0] Δ metric for WISE 3.4um (always "0")
46 A1 --- l_delta4.6 Limit flag for delta4.6
47 I1 --- delta4.6 [0] Δ metric for WISE 4.6um (always "0")
49 A1 --- l_sigma3.4 Limit flag for sigma3.4
50- 51 I2 --- sigma3.4 [3/27]? Significance level of W1 band
variability
53 A1 --- l_sigma4.6 Limit flag for sigma4.6
54- 55 I2 --- sigma4.6 [3/19]? Significance level of W2 band
variability
57- 58 A2 --- Note Note (1)
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Note (1): "RV" means detection of rapid MIR variability, i.e., a significant
(>3σ) variability in either of the W1 and W2 bands.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 26-Oct-2021