J/A+A/575/A80 FIR photometry of 3CR galaxies (Podigachoski+, 2015)
Star formation in z>1 3CR host galaxies as seen by Herschel.
Podigachoski P., Barthel P.D., Haas M., Leipski C., Wilkes B.,
Kuraszkiewicz J., Westhues C., Willner S.P., Ashby M.L.N., Chini R.,
Clements D.L., Fazio G.G., Labiano A., Lawrence C., Meisenheimer K.,
Peletier R.F., Siebenmorgen R., Verdoes Kleijn G.
<Astron. Astrophys., 575, A80-80 (2015)>
=2015A&A...575A..80P 2015A&A...575A..80P
ADC_Keywords: Galaxies, radio ; Photometry, infrared
Keywords: galaxies: active - galaxies: high-redshift -
galaxies: star formation - infrared: galaxies
Abstract:
We present Herschel (PACS and SPIRE) far-infrared (FIR) photometry of
a complete sample of z>1 3CR sources, from the Herschel guaranteed
time project The Herschel Legacy of distant radio-loud AGN. Combining
these with existing Spitzer photometric data, we perform an infrared
(IR) spectral energy distribution (SED) analysis of these landmark
objects in extragalactic research to study the star formation in the
hosts of some of the brightest active galactic nuclei (AGN) known at
any epoch. Accounting for the contribution from an AGN-powered warm
dust component to the IR SED, about 40% of our objects undergo
episodes of prodigious, ULIRG-strength star formation, with rates of
hundreds of solar masses per year, coeval with the growth of the
central supermassive black hole. Median SEDs imply that the quasar and
radio galaxy hosts have similar FIR properties, in agreement with the
orientation-based unification for radio-loud AGN. The star-forming
properties of the AGN hosts are similar to those of the general
population of equally massive non-AGN galaxies at comparable
redshifts, thus there is no strong evidence of universal quenching of
star formation (negative feedback) within this sample. Massive
galaxies at high redshift may be forming stars prodigiously,
regardless of whether their supermassive black holes are accreting or
not.
Description:
The data for this work were obtained as part of our Herschel
guaranteed time project The Herschel Legacy of distant radio-loud AGN
(PI: Barthel, 38h of observations). Five objects were observed as part
of another Herschel programme (PI: Seymour).
Photometric observations were carried out with PACS in the scan-map
observational mode, both in the blue (70um, 5" angular resolution)
and in the red (160um, 11" angular resolution) bands.
SPIRE photometric observations were carried out in small scan-map
observational mode, at 250 (18.2" angular resolution), 350 (24.9"
angular resolution) and 500um (36.3" angular resolution).
The FIR photometry of all 3CR sources in our work was supplemented
with MIR photometry obtained with the Spitzer Space Telescope during
three Spitzer GT observing programmes (PI: G. Fazio) in six bands,
using the instruments IRAC, IRS-16 peak-up array and MIPS.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 81 62 Summary of selected properties of the high-z
3CR sample studied in this work
table2.dat 134 62 Herschel and Spitzer photometry of the 3CR objects
studied in this work
table4.dat 78 61 Physical parameters estimated from the SED fitting
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See also:
VIII/1 : The 3C and 3CR Catalogues (Edge+ 1959-1962)
Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Name Name of object (in 3C or 4C)
9 A1 --- Src [a] Source of Herschel data (1)
11- 13 A3 --- Type AGN type: QSR=quasar, or RG=radio galaxy
15- 18 F4.2 --- z [1/2.5] Redshift
20- 21 I2 h RAh Right ascension (J2000)
23- 24 I2 min RAm Right ascension (J2000)
26- 30 F5.2 s RAS Right ascension (J2000)
32 A1 --- DE- Declination sign (J2000)
33- 34 I2 deg DEd Declination (J2000)
36- 37 I2 arcmin DEm Declination (J2000)
39- 43 F5.2 arcsec DEs Declination (J2000)
45- 48 F4.1 [W/Hz] log(Lr) Log of 178MHz luminosity (in observer's frame)
50- 59 I10 --- PObsID1 Herschel/PACS first ObsIDs
60 A1 --- --- [/]
61- 70 I10 --- PObsID2 Herschel/PACS second ObsIDs
72- 81 I10 --- SPObsID Herschel/SPIRE ObsIDs
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Note (1): the data were obtained as part of our Herschel Guaranteed Time
project "The Herschel Legacy of distant radio-loud AGN" (PI: Barthel,
38 hours of observations). Five objects marked "a" were observed as
part of another Herschel programme (PI: Seymour)
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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- 8 A8 --- Name Name of object (in 3C or 4C)
10 A1 --- l_F3.6 Limit of F3.6um (3σ upper limit)
11- 14 I4 Jy F3.6 Spitzer/IRAC Flux in 3.6um band
16- 18 I3 Jy e_F3.6 ? 1σ rms uncertainty on F3.6
20 A1 --- l_F4.5 Limit flag on F4.5um (3σ upper limit)
21- 24 I4 Jy F4.5 Spitzer/IRAC Flux in 4.5um band
26- 28 I3 Jy e_F4.5 ? 1σ rms uncertainty on F4.5
30- 33 I4 Jy F5.8 Spitzer/IRAC Flux in 5.8um band
35- 37 I3 Jy e_F5.8 1σ rms uncertainty on F5.8
39 A1 --- l_F8.0 Limit flag on F8.0um (3σ upper limit)
40- 43 I4 Jy F8.0 Spitzer/IRAC Flux in 8.0um band
45- 47 I3 Jy e_F8.0 ? 1σ rms uncertainty on F8.0
49 A1 --- l_F16 Limit flag on F16um (3σ upper limit)
50- 54 I5 Jy F16 ?=- Spitzer/IRS16 flux in 16um band
56- 59 I4 Jy e_F16 ? 1σ rms uncertainty on F16
61 A1 --- l_F24 Limit flag on F24um (3σ upper limit)
62- 66 I5 Jy F24 Spitzer/MIPS flux in 24um band
68- 71 I4 Jy e_F24 ? 1σ rms uncertainty on F24
73 A1 --- l_F70 Limit flag on F70um (3σ upper limit)
74- 77 F4.1 Jy F70 ?=- Herschel/PACS flux in 70um band
79- 81 F3.1 Jy e_F70 ? 1σ rms uncertainty on F70
82 A1 --- n_F70 [b] contamination in F70um (2)
84 A1 --- l_F160 Limit flag on F160um (3σ upper limit)
85- 89 F5.1 Jy F160 ?=- Herschel/PACS flux in 160um band
91- 94 F4.1 Jy e_F160 ? 1σ rms uncertainty on F160
95 A1 --- n_F160 [b] contamination in F160um (2)
97 A1 --- l_F250 Limit flag on F250um (3σ upper limit)
98-102 F5.1 Jy F250 ?=- Herschel/SPIRE flux in 250um band
104-107 F4.1 Jy e_F250 ? 1σ rms uncertainty on F250
108 A1 --- n_F250 [ab] low S/N or contamination in F250um (2)
110 A1 --- l_F350 Limit flag on F350um (3σ upper limit)
111-115 F5.1 Jy F350 ?=- Herschel/SPIRE flux in 350um band
117-120 F4.1 Jy e_F350 ? 1σ rms uncertainty on F350
121 A1 --- n_F350 [ab] low S/N or contamination in F350um (2)
123 A1 --- l_F500 Limit flag on F500um (3σ upper limit)
124-128 F5.1 Jy F500 ?=- Herschel/SPIRE flux in 500um band
130-133 F4.1 Jy e_F500 ? 1σ rms uncertainty on F500
134 A1 --- n_F500 [ab] low S/N or contamination in F500um (2)
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Note (2): Notes as follows:
a = less than 3σ detection entering our SED fitting routine
b = photometric measurement hindered by the presence of a nearby source
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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 A1 --- f_Name [*] *: Objects detected in fewer than
three Herschel bands
3- 10 A8 --- Name Name of object (in 3C or 4C)
11- 13 A3 --- n_Name [abcd, ] Individual note (3)
15 A1 --- l_LAGN Limit flag on LAGN
16- 19 F4.1 10+12Lsun LAGN IR luminosity of the AGN powered dust
emission (4)
21- 23 F3.1 10+12Lsun E_LAGN ? Error on LAGN (upper value)
25- 27 F3.1 10+12Lsun e_LAGN ? Error on LAGN (lower value)
29 A1 --- l_LSF Limit flag on LSF
30- 32 F3.1 10+12Lsun LSF IR luminosity of the modified blackbody
component (5)
34- 36 F3.1 10+12Lsun E_LSF ? Error on LSF (upper value)
38- 40 F3.1 10+12Lsun e_LSF ? Error on LSF (lower value)
42 A1 --- l_SFR Limit flag on SFR
43- 45 F3.1 10+2Msun/yr SFR Star formation rate (6)
47- 49 F3.1 10+2Msun/yr E_SFR ? Error on SFR (upper value)
51- 53 F3.1 10+2Msun/yr e_SFR ? Error on SFR (lower value)
55- 57 F3.1 10+8Msun Md ? Mass of the modified blackbody component
59- 61 F3.1 10+8Msun E_Md ? Error on Md (upper value)
63- 65 F3.1 10+8Msun e_Md ? Error on Md (lower value)
67- 70 F4.1 K Td ? Temperature of the modified blackbody
component
72- 74 F3.1 K E_Td ? Error on Td (upper value)
76- 78 F3.1 K e_Td ? Error on Td (lower value)
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Note (3): Notes as follows:
a = For this radio galaxy, a blackbody component (1300K) was included in the
SED fitting
b = This object was included in the stacking of non-detected radio galaxies
c = This object was included in the stacking of non-detected quasars
d = The emissivity index of the cold dust component, β, was estimated for
this object
Note (4): IR luminosity (integrated between 1um and 1000um) of the AGN powered
dust emission, i.e. torus component and sum of torus and hot dust components
for RGs and QSRs, respectively
Note (5): IR luminosity (integrated between 8um and 1000um) of the modified
blackbody component (β=1.6) presumably powered by star formation
activity in the AGN host galaxy
Note (6): determined from the IR luminosity in LSF using the calibration
derived in Kennicutt (1998ARA&A..36..189K 1998ARA&A..36..189K).
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 22-Jun-2015