J/A+A/439/487 Nuker law fits of radio galaxies (De Ruiter+, 2005)
Are radio galaxies and quiescent galaxies different?
Results from the analysis of HST brightness profiles.
De Ruiter H.R., Parma P., Capetti A., Fanti R., Morganti R., Santantonio L.
<Astron. Astrophys., 439, 487-496 (2005)>
=2005A&A...439..487D 2005A&A...439..487D
ADC_Keywords: Galaxies, radio ; Redshifts
Keywords: Galaxies: active - Galaxies: elliptical and lenticulars, cD -
Galaxies: nuclei
Abstract:
We present Nuker law fits of brightness profiles of a number of radio
galaxies that were observed with the HST. The data on B2 radio
galaxies were described in Capetti et al. (2000A&A...362..871C 2000A&A...362..871C), while
a number of 3C galaxies with FR II radio structure were taken from the
HST archive. The profiles are compared with other samples of early
type galaxies, taken from the literature. We find that radio galaxies
always have "core"-type profiles, i.e. a shallow profile in the inner
part of the galaxy, while radio-quiescent ellipticals may either have
"core"-type or "power-law" type profiles.
Description:
Nuker-model parameters are given for three sets of galaxies. The
parameters were derived from Nuker-law fits of the inner parts of the
brightness profiles. All observational data are based on HST images.
We present the data for 1) the subset of B2 radio galaxies with
central dust and 2) without central dust (see Capetti et al.,
2000A&A...362..871C 2000A&A...362..871C), and 3) 3C (FR II type) radio galaxies with
images available in the HST archive. We also give general information,
including new data on radio power, on two comparison samples: nearby
early type galaxies discussed by Faber et al. (1997AJ.....114.1771F)
and brightest cluster galaxies that were analysed by Laine et al.
(2003AJ.....125..478L).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 102 17 Nuker law parameters of B2 radio galaxies
with central dust
table2.dat 102 22 Nuker law parameters of B2 radio galaxies
without central dust
table3.dat 93 9 Nuker law parameters of 3CR radio galaxies
of FR type II
table4.dat 46 33 Faber et al. (1997AJ.....114.1771F) and
Laine et al. (2003AJ.....125..478L) basic data
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Byte-by-byte Description of file: table1.dat table2.dat table3.dat
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Bytes Format Units Label Explanations
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1- 10 A10 --- Name Name of radio source
12- 15 F4.2 --- alpha Nuker parameter α (1)
17- 20 F4.2 --- e_alpha 1-{sigme} uncertainty of alpha
22- 25 F4.2 --- beta Nuker parameter β (1)
27- 30 F4.2 --- e_beta 1-{sigme} uncertainty of beta
32- 36 F5.2 --- gamma Nuker parameter γ (1)
38- 41 F4.2 --- e_gamma 1-{sigme} uncertainty of gamma
43- 47 F5.3 arcsec rb Nuker parameter rb (1)
49- 53 F5.3 arcsec e_rb 1-{sigme} uncertainty of rb
55- 59 F5.2 mag/arcsec2 mub Nuker parameter µb (1)
61- 64 F4.2 mag/arcsec2 e_mub 1-{sigme} uncertainty of mub
66- 71 F6.4 --- z Redshift
73- 77 F5.2 [W/Hz] log(Pt) logarithm of total radio power (at 1.4GHz)
79- 84 F6.2 mag VMAG Absolute V magnitude of galaxy
86- 89 F4.1 % b4 ?=- Deviation from pure ellipse in %
91- 93 F3.1 % e_b4 ?=- 1-{sigme} uncertainty of b4 in %
95-102 A8 --- OName Alternative NGC or 3C name
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Note (1): The "Nuker profile" is an empirical law introduced by Lauer et al.
(1995AJ....110.2622L 1995AJ....110.2622L). In terms of magnitudes the Nuker law reads:
µ(r) = µb - [(β-γ)/α]*2.5log2
+ 2.5*γ*log(r/rb)
+ 2.5*[(β-γ)/α]*log(1+(r/rb)α)
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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- 9 A9 --- Galaxy Name of galaxy (1)
11- 16 F6.4 --- z redshift
18- 23 F6.2 mag VMAG Absolute magnitude of galaxy
25 A1 --- l_log(Pt) Upper limit flag (<) of radio power (2)
26- 30 F5.2 [W/Hz] log(Pt) ?=- logarithm of total radio power (at 1.4GHz)
32 A1 --- Sample F: Faber+ (1997); L: Laine+ (2003) (1)
34- 46 A13 --- Info Information on radio source (3)
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Note (1): Galaxy names taken from the original papers by Faber et al.
(1997AJ.....114.1771F) and Laine et al. (2003AJ.....125..478L).
Note (2): 3-{sigme} detection limit is 1.35mJy (NVSS).
Note (3): Some objects could not be searched for radio emission (e.g. because
too far to the south for NVSS, or because a precise position is
lacking). Galaxies with VMAG>-17 were excluded from the analysis.
Abell 168 was excluded because of a large discrepancy between the fit
parameter γ and the slope directly measured at 0.05 arcsec.
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Acknowledgements: Hans de Ruiter, deruiter(at)bo.astro.it
History:
* 22-Sep-2005: Original table
* 27-Oct-2005: in table 2, 2nd row, B2 0120+33 corrected into B2 0120+32
(End) Hans de Ruiter [INAF-OAB, Bologna], Patricia Vannier [CDS] 22-Sep-2005