Flat-Spectrum Radio Sources with Faint Optical Counterparts

Stickel, M.; Rieke, G. H.; Kuehr, H.; Rieke, M. J.

doi:10.1086/177714

Cited by 78 publications

(121 citation statements)

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“…B0742+103: neither Stickel et al (1996) nor de Vries et al (1995) were able to identify the host of this relatively bright radio source. Our UT1 image (Fig.…”

Section: B0407-658mentioning

confidence: 86%

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GPS radio sources: new optical observations and an updated master list

Labiano

Barthel²,

O’Dea

et al. 2006

A&A

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Aims. We identify optical counterparts, address uncertain identifications and measure previously unknown redshifts of the host galaxies of candidate GPS radio sources, and study their stellar populations. Methods. Long slit spectroscopy and deep optical imaging in the B, V and R bands, obtained with the Very Large Telescope. Results. We obtain new redshifts for B0316+161, B0407-658, B0904+039, B1433-040, and identify the optical counterparts of B0008-421 and B0742+103. We confirm the previous identification for B0316+161, B0407-658, B0554-026, and B0904+039, and find that the previous identification for B0914+114 is incorrect. Using updated published radio spectral information, we classify as non GPS the following sources: B0407-658, B0437-454, B1648+015. The optical colors of typical GPS sources are consistent with single instantaneous burst stellar population models but do not yield useful information on age or metallicity. A new master list of GPS sources is presented.

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“…B0742+103: neither Stickel et al (1996) nor de Vries et al (1995) were able to identify the host of this relatively bright radio source. Our UT1 image (Fig.…”

Section: B0407-658mentioning

confidence: 86%

“…We measure z = 0.907 based on five lines. Stickel et al (1996) identified the optical counterpart of this radio source as a galaxy. The spectrum (Fig.…”

Section: B0008-421mentioning

confidence: 99%

GPS radio sources: new optical observations and an updated master list

Labiano

Barthel²,

O’Dea

et al. 2006

A&A

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“…References. References for the redshifts of the lenses and sources: (a) Browne et al (1993); Stickel & Kuehr (1993);Carilli et al (1993); (b) Cohen et al (2003); (c) Lubin et al (2000); (d) Kochanek et al (1997); Oscoz et al (1997); (e) Kneib et al (2000); (f) Bade et al (1997); (g) Eigenbrod et al (2007); (h) Jakobsson et al (2005); (i) Lidman et al (2000); (j) Smette et al (1995); (k) Tonry (1998); (l) Weymann et al (1980); (m) Tonry (1998); (n) Patnaik et al (1992); (o) Auger et al (2008); (p) Chavushyan et al (1997); (q) Jaunsen & Hjorth (1997); Fassnacht & Cohen (1998); (r) Fassnacht & Cohen (1998); (s) Myers et al (1995); (t) Fassnacht et al (1996); (u) Eigenbrod et al (2007); (v) Wisotzki et al (1996). …”

Section: Datamentioning

confidence: 99%

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

Sluse

Chantry

Magain

et al. 2012

A&A

121

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Gravitationally lensed quasars can be used as powerful cosmological and astrophysical probes. We can (i) infer the Hubble constant H 0 based on the so-called time-delay technique, (ii) unveil substructures along the line-of-sight toward distant galaxies, and (iii) compare the shape and the slope of baryons and dark matter distributions in the inner regions of galaxies. To reach these goals, we need highaccuracy astrometry of the quasar images relative to the lensing galaxy and morphology measurements of the lens. In this work, we first present new astrometry for 11 lenses with measured time delays, namely, JVAS B0218+357, SBS 0909+532, RX J0911.4+0551, FBQS J0951+2635, HE 1104-1805, PG 1115+080, JVAS B1422+231, SBS 1520+530, CLASS B1600+434, CLASS B1608+656, and HE 2149-2745. These measurements proceed from the use of the Magain-Courbin-Sohy (MCS) deconvolution algorithm applied in an iterative way (ISMCS) to near-IR HST images. We obtain a typical astrometric accuracy of about 1-2.5 mas and an accurate shape measurement of the lens galaxy. Second, we combined these measurements with those of 14 other lensing systems, mostly from the COSMOGRAIL set of targets, to present new mass models of these lenses. The modeling of these 25 gravitational lenses led to the following results: 1) in four double-image quasars (HE0047-1746, J1226-006, SBS 1520+530, and HE 2149-2745), we show that the influence of the lens environment on the time delay can easily be quantified and modeled, hence putting these lenses with high priority for time-delay determination; 2) for quadruple-image quasars, the difficulty often encountered in reproducing the image positions to milli-arcsec accuracy (astrometric anomaly problem) is overcome by explicitly including the nearest visible galaxy/satellite in the lens model. However, one anomalous system (RXS J1131-1231) does not show any luminous perturber in its vicinity, and three others (WFI 2026-4536, WFI 2033, and B2045+265) have problematic modeling. These four systems are the best candidates for a pertubation by a dark matter substructure along the line-of-sight; 3) we revisit the correlation between the position angle (PA) and ellipticity of the light and of the mass distribution in lensing galaxies. As in previous studies, we find a significant correlation between the PA of the light and of the mass distributions. However, in contrast with these same studies, we find that the ellipticity of the light and of the mass also correlate well, suggesting that the overall spatial distribution of matter is not very different from the baryon distribution in the inner ∼5 kpc of lensing galaxies. This offers a new test for high-resolution hydrodynamical simulations.

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“…However, detections at radio-wavelengths (e.g., Smith & Spinrad 1980;Rieke et al 1982;Ledden & O'Dell 1983;Webster et al 1995;Stickel et al 1996;Najita et al 2000;Brotherton et al 2001), as well as in the near infrared (Beichman et al 1998), and in the X-ray band (e.g., Kim & Elvis 1999;Vignali et al 2000;Nakanishi et al 2000) revealed the existence of a substantial population of QSOs with unexpected red colours. On the basis of a complete sample of radio sources from the Parkes Half-Jansky FlatSpectrum survey, Webster and co-workers (Webster et al 1995;Drinkwater et al 1997;Masci et al 1999;Francis et al 2000) found a strong population of red sources, some having extremely red B − K colours.…”

Section: Red Qsosmentioning

confidence: 99%

A QSO survey via optical variability and zero proper motion in the M 92 field

Meusinger¹,

Brunzendorf²

2001

A&A

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Abstract. The combination of variability and proper motion constraints (VPM search) is believed to provide an efficient yet unconventional search strategy for QSOs with selection effects quite different from conventional optical QSO surveys. We performed a VPM QSO search in a 10 square degrees field around M 92 on 162 selected digitised Schmidt plates in the Johnson B band with a time-baseline of more than three decades. In Paper I, we constructed a sample of VPM QSO candidates with B ≤ 19.7. The spectroscopic follow-up observations revealed 58 QSOs and 7 Seyfert 1 galaxies as well as 27 narrow-emission line galaxies. We present the lowresolution spectra and the data for the QSOs and Seyfert galaxies: AGN types, accurate positions, redshifts, mean B magnitudes, and colour indices, along with the selection parameters of the VPM search, i.e., indices for variability, proper motion, and image structure. The redshifts cover the interval 0 < ∼ z < ∼ 3; absolute magnitudes are in the range −21 < ∼ MB < ∼ −29. The statistical properties of the resulting QSO sample are studied in detail. No significant differences were found between our VPM QSO sample and published QSO samples from multicolour or spectroscopic surveys. The fraction of QSOs with unusual colours is estimated to be less than 5 per cent within the magnitude range B ≤ 19.7.

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Flat-Spectrum Radio Sources with Faint Optical Counterparts

Cited by 78 publications

References 0 publications

GPS radio sources: new optical observations and an updated master list

GPS radio sources: new optical observations and an updated master list

COSMOGRAIL: the COSmological MOnitoring of GRAvItational Lenses

A QSO survey via optical variability and zero proper motion in the M 92 field

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