J/ApJ/755/171 [CII]158um line fluxes of AGN from Herschel (Sargsyan+, 2012)
[C II] 158 µm luminosities and star formation rate in dusty starbursts
and active galactic nuclei.
Sargsyan L., Lebouteiller V., Weedman D., Spoon H., Bernard-Salas J.,
Engels D., Stacey G., Houck J., Barry D., Miles J., Samsonyan A.
<Astrophys. J., 755, 171 (2012)>
=2012ApJ...755..171S 2012ApJ...755..171S
ADC_Keywords: Active gal. nuclei ; Redshifts ; Equivalent widths ;
Spectra, infrared
Keywords: galaxies: active; galaxies: distances and redshifts;
galaxies: starburst; infrared: galaxies
Abstract:
Results are presented for [CII] 158µm line fluxes observed with the
Herschel PACS instrument in 112 sources with both starburst and active
galactic nucleus (AGN) classifications, of which 102 sources have
confident detections. Results are compared with mid-infrared spectra
from the Spitzer Infrared Spectrometer and with Lir from IRAS
fluxes; AGN/starburst classifications are determined from equivalent
width of the 6.2µm polycyclic aromatic hydrocarbon (PAH) feature.
It is found that the [CII] line flux correlates closely with the flux
of the 11.3µm PAH feature independent of AGN/starburst
classification, log[f([CII]158µm)/f(11.3µmPAH)]=-0.22±0.25. It
is concluded that the [CII] line flux measures the photodissociation
region associated with starbursts in the same fashion as the PAH
feature. A calibration of star formation rate (SFR) for the starburst
component in any source having [CII] is derived comparing [CII]
luminosity L([CII]) to Lir with the result that
logSFR=logL([CII)])-7.08±0.3, for SFR in M☉/yr and L([CII]) in
L☉. The decreasing ratio of L([CII]) to Lir in more luminous
sources (the "[CII] deficit") is shown to be a consequence of the
dominant contribution to Lirarising from a luminous AGN component
because the sources with the largest Lir and smallest L([CII])/Lir
are AGNs.
Description:
The 112 sources in our observing program (Herschel Photodetector Array
Camera and Spectrometer (PACS) proposal OT1dweedman1) are taken from
the 301 sources in Sargsyan et al. (2011, Cat. J/ApJ/730/19). All
[CII]158um observations were made using PACS line spectroscopy in
point-source chop nod mode with medium throw. A single repetition
cycle was used for all but 20 sources, giving total observing time for
the program of 20.2hr for 112 sources.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 131 112 [CII] line fluxes and luminosities
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See also:
VI/139 : Herschel Observation Log (Herschel Science Centre, 2013)
J/A+A/551/A100 : Panchromatic SED of Herschel sources (Berta+, 2013)
J/AJ/143/125 : SED of 113 dust-obscured galaxies at z∼2 (Melbourne+, 2012)
J/MNRAS/423/197 : MIPS photometry for Herschel SAG2 Programs (Bendo+, 2012)
J/ApJ/730/19 : IR spectra and SEDs for starbursts and AGNs (Sargsyan+, 2011)
J/MNRAS/409/2 : Herschel sources SED model parameters (Rowan-Robinson+, 2010)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 3 I3 --- Seq [1/112] Running sequence number
5- 28 A24 --- Name Target name
30 A1 --- f_Name [j] Observation on 2 cycles (1)
32- 33 I2 h RAh Hour of right ascension (J2000)
34- 35 I2 min RAm Minute of right ascension (J2000)
36- 40 F5.2 s RAs Second of right ascension (J2000)
41 A1 --- DE- Sign of declination (J2000)
42- 43 I2 deg DEd Degree of declination (J2000)
44- 45 I2 arcmin DEm Arcminute of declination (J2000)
46- 49 F4.1 arcsec DEs Arcsecond of declination (J2000)
51- 56 F6.4 --- z [0.003/0.4] Redshift
58 A1 --- l_EW Limit flag on EW
60- 64 F5.3 um EW [0.001/0.6] Rest-frame equivalent width of
6.2um PAH emission feature (2)
66 A1 --- f_EW [kl] Flag on spectrum (1)
68 A1 --- l_F158 Limit flag on F158
70- 77 E8.3 W/m2 F158 Total flux of [CII] 158um emission line (3)
79 A1 --- f_F158 [i] Asymmetric CII line (1)
81- 85 F5.1 --- S/N [0.1/249] Signal-to-noise ratio (4)
87 A1 --- f_S/N [h] displaced spaxel (1)
89 A1 --- l_F/11 Limit flag on F/11
91- 95 F5.2 [-] F/11 Ratio of flux in [CII] 158um to flux of
PAH 11.3um emission feature (5)
97 A1 --- f_F/11 [l] PAH measure from Wu et al. (1)
99 A1 --- l_F/7 Limit flag on F/7
101-105 F5.2 [-] F/7 [-4.1/-1.6] Ratio FCII/νfν(7.8um) (5)
107 A1 --- l_L158 Limit flag on L158
109-112 F4.2 [Lsun] L158 [6.12/9.26] [CII] 158um emission line
luminosity (6)
114 A1 --- l_L158/Lir Limit flag on L158/Lir
116-120 F5.2 [-] L158/Lir [-4.3/-2.5] Ratio of [CII] IR luminosity (7)
122-131 I10 --- ObsId Herschel observation number
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Note (1): Flag as follows:
h = Brightest spaxel displaced one spaxel from central 3,3 spaxel.
(a "spaxel" means "equivalent spatial pixel")
i = [CII] line profile is asymmetric or has component structure so total line
flux is integrated flux including all components rather than flux within a
single Gaussian fit.
j = Observation made with two repetition cycles of line spectroscopy point
source chop nod mode; all observations without note made with single cycle.
k = IRS spectrum shows 9.7µm silicate feature in absorption.
l = For these four sources, spectra are not in CASSIS because IRS spectra
obtained in mapping mode; PAH measures from Wu et al.
(2009ApJ...701..658W 2009ApJ...701..658W).
Note (2): Rest-frame equivalent width of 6.2µm PAH emission feature from
Sargsyan et al. 2011 (J/ApJ/730/19) used to classify source as AGN,
composite, or starburst.
Note (3): Total flux of [CII] 158µm emission line using Gaussian fit to
line for simple profiles and integrated flux of line for complex
profiles (flagged "i" in the next column). Line flux listed is the
total flux observed within the 9 "spaxels" (equivalent spatial pixels)
centered on the brightest spaxel, increased by a correction factor of
1.16-1.21 to include flux that would fall outside these spaxels for
an unresolved source. The correction factor adopted for the range of
observed [CII] wavelengths from 160µm to 210µm is
1.16(λ/158µm)0.17. Uncertainties of individual fits given
by S/N; systematic uncertainty for all fluxes depends on PACS flux
calibration, estimated as ±12% in the PACS Spectroscopy performance
and calibration document PICC-KL-TN-041.
Note (4): Signal-to-noise ratio of total line flux in brightest "spaxel"
(equivalent spatial pixel), using 1σ uncertainty of profile fit.
Note (5): From Sargsyan et al. 2011 (J/ApJ/730/19).
Note (6): [CII] 158µm emission line luminosity using luminosity
distances determined for H0=71km/s/Mpc, ΩM=0.27, and
ΩΛ=0.73, from Wright (2006PASP..118.1711W 2006PASP..118.1711W):
http://www.astro.ucla.edu/wright/CosmoCalc.html
[logLCII(solar)=logLCII(W)-26.59].
Note (7): Ratio of [CII] luminosity to Lir using Lir given in Sargsyan
et al. 2011 (J/ApJ/730/19) from fir determined as in Sanders &
Mirabel (1996ARA&A..34..749S 1996ARA&A..34..749S),
fir=1.8x10-11[13.48f(12)+5.16f(25)+2.58f(60)+f(100)] erg/cm2/s
using IRAS flux densities f(λ) at 12, 25, 60, and 100µm.
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History:
From electronic version of the journal
(End) Emmanuelle Perret [CDS] 13-Mar-2014