2004A&A...413...97G


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.12CET00:38:49

2004A&A...413...97G - Astronomy and Astrophysics, volume 413, 97-105 (2004/1-1)

The nuclear region of low luminosity flat radio spectrum sources. II. Emission-line spectra.

GONCALVES A.C. and SEROTE ROOS M.

Abstract (from CDS):

We report on the spectroscopic study of 19 low luminosity Flat Radio Spectrum (LL FRS) sources selected from Marcha's et al. (1996MNRAS.281..425M) 200mJy sample. In the optical, these objects are mainly dominated by the host galaxy starlight. After correcting the data for this effect, we obtain a new set of spectra clearly displaying weak emission lines; such features carry valuable information concerning the excitation mechanisms at work in the nuclear regions of LL FRS sources. We have used a special routine to model the spectra and assess the intensities and velocities of the emission lines; we have analyzed the results in terms of diagnostic diagrams. Our analysis shows that 79% of the studied objects harbour a Low Ionization Nuclear Emission-line Region (or LINER) whose contribution was swamped by the host galaxy starlight. The remaining objects display a higher ionization spectrum, more typical of Seyferts; due to the poor quality of the spectra, it was not possible to identify any possible large Balmer components. The fact that we observe a LINER-type spectrum in LL FRS sources supports the idea that some of these objects could be undergoing an ADAF phase; in addition, such a low ionization emission-line spectrum is in agreement with the black hole mass values and sub-Eddington accretion rates published for some FRS sources.

Abstract Copyright:

Journal keyword(s): galaxies: active - galaxies: BL Lacertae objects: general - galaxies: general

CDS comments: p. 104 : S5 2116+81 = CJF B2116+818

Simbad objects: 22

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Number of rows : 22

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 NVSS J003808+230327 rG 00 38 08.10240 +23 03 28.4400           ~ 25 1
2 NGC 315 LIN 00 57 48.88335 +30 21 08.8122 12.80 12.20 11.16 11.26   ~ 683 2
3 4C 31.04 rG 01 19 35.00346907 +32 10 50.0583319   16 14.5     ~ 209 1
4 8C 0149+710 BLL 01 53 25.8474314588 +71 15 06.539151303     15.50     ~ 65 1
5 ICRF J065510.0+410010 QSO 06 55 10.02473 +41 00 10.1598   14.6   9.37   ~ 56 1
6 2MASX J07332855+5605422 G 07 33 28.6155259744 +56 05 41.755946814           ~ 23 1
7 7C 073311.80+594748.00 Bla 07 37 30.08697865 +59 41 03.1943714   15.5   11.8   ~ 55 1
8 NVSS J085319+682817 rG 08 53 18.8914357643 +68 28 19.026307038   14.8       ~ 21 1
9 ICRF J090615.5+463619 Sy1 09 06 15.53964568 +46 36 19.0254139   16.80 16.08     ~ 37 1
10 ICRF J114722.1+350107 Sy2 11 47 22.13056 +35 01 07.5226   17.89 16.83 10.26   ~ 146 1
11 7C 114610.00+594129.00 Bla 11 48 50.35825 +59 24 56.3820   12.9   11.57   ~ 201 1
12 M 87 BiC 12 30 49.42338230 +12 23 28.0438581 10.16 9.59 8.63   7.49 ~ 6033 3
13 NVSS J124310+731600 rG 12 43 11.2160930587 +73 15 59.253486477           ~ 22 1
14 ICRF J124733.3+672316 QSO 12 47 33.32954415 +67 23 16.4507419           ~ 68 1
15 6C 155808+593251 QSO 15 59 01.7059221 +59 24 21.846474   16       ~ 33 1
16 4C 30.31 rG 17 00 45.2306715604 +30 08 12.865819789   15.00 14.3     ~ 67 0
17 2MASX J17052935+2216075 Sy2 17 05 29.3303596159 +22 16 07.586767246           ~ 21 0
18 NGC 6521 Sy1 17 55 48.4338041826 +62 36 44.127834813   14.3   9.3   ~ 56 1
19 2MASX J20180125-5539312 Sy2 20 18 01.2945368877 -55 39 31.591523913   15.5       ~ 50 0
20 2MAXI J2115+821 Sy1 21 14 01.1716311384 +82 04 48.338015583           ~ 105 1
21 ICRF J220421.1+363237 QSO 22 04 21.10048271 +36 32 37.0916492       12.88   ~ 24 1
22 PKS 2320+203 rG 23 23 20.3427468174 +20 35 23.477545374   15.5 15.5     ~ 31 1

    Equat.    Gal    SGal    Ecl

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2019.11.12-00:38:49

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