2014A&A...570A..96S


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.08CEST03:44:42

2014A&A...570A..96S - Astronomy and Astrophysics, volume 570A, 96-96 (2014/10-1)

GTC spectra of z ≃ 2.3 quasars: comparison with local luminosity analogs.

SULENTIC J.W., MARZIANI P., DEL OLMO A., DULTZIN D., PEREA J. and NEGRETE C.A.

Abstract (from CDS):

The advent of 8-10m class telescopes for the first time makes it possible to compare in detail quasars with similar luminosity and very different redshifts. We conducted a search for z-dependent gradients in line-emission diagnostics and derived physical properties by comparing, in a narrow bolometric luminosity range (logL ∼46.1±0.4[erg/s]), some of the most luminous local z<0.6 quasars with some of the lowest luminosity sources yet found at redshift z=2.1-2.5. Moderate signal-to-noise ratio spectra for 22 high-redshift sources were obtained with the 10.4m Gran Telescopio Canarias (GTC), for which the HST (largely the Faint Object Spectrograph) archive provides a low-redshift control sample. We compared the spectra in the context of the 4D Eigenvector 1 formalism, meaning that we divided both source samples into highly accreting population A and population B sources accreting at a lower rate. CIVλ1549, the strongest and most reliable diagnostic line, shows very similar properties at both redshifts, which confirms the CIVλ1549 profile differences at high redshift between populations A and B, which are well established in local quasars. The CIVλ1549 blueshift that appears quasi-ubiquitous in higher L sources is found in only half (population A) of the quasars observed in the two samples. A CIVλ1549 evolutionary Baldwin effect is certainly disfavored. We find evidence for lower metallicity in the GTC sample that may point toward a gradient with z. No evidence for a gradient in MBH or L/LEdd is found. Spectroscopic differences established at low z are also present in much higher redshift quasars. Our results on the CIVλ1549 blueshift suggest that it depends both on source luminosity and L/LEdd. Given that our samples involve sources with very similar luminosity, the evidence for a systematic metallicity decrease, if real, points toward an evolutionary effect. Our samples are not large enough to effectively constrain possible changes of MBH or L/LEdd with redshift. The two samples appear representative of a slowly evolving quasar population that is most likely present at all redshifts.

Abstract Copyright:

Journal keyword(s): quasars: emission lines - quasars: supermassive black holes - ISM: abundances - line: profiles - cosmology: observations

VizieR on-line data: <Available at CDS (J/A+A/570/A96): table12.dat sp/*>

Simbad objects: 31

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Number of rows : 31

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 Mrk 1502 Sy1 00 53 34.9326560879 +12 41 35.927159668   14.41 14.03     ~ 1034 1
2 GD 24 WD* 02 13 05.3882500684 +16 43 12.483358492   16.0       DA 9 0
3 Feige 34 HS* 10 39 36.7377085527 +43 06 09.209752646 9.613 10.91 11.14 11.319 11.464 sdOp 604 0
4 GD 140 WD* 11 37 05.1038329295 +29 47 58.292363897 11.47 12.42 12.45 12.73 12.714 DA2.2 211 0
5 QSO B1216-1046 QSO 12 18 48.6983145583 -11 03 32.602004886     21.1     ~ 6 0
6 QSO B1232-1059 QSO 12 34 39.1030193995 -11 16 23.309395071     20.7     ~ 6 0
7 QSO B1232-1113 QSO 12 35 02.4667492980 -11 30 28.624979541     20.9     ~ 7 0
8 [VV2006] J123742.6+621811 QSO 12 37 42.529 +62 18 11.70 22.49 22.12 22.097 21.8 21.575 ~ 26 0
9 QSO B1257+357 QSO 12 59 35.3396254879 +35 30 52.178116658   20.89 20.78     ~ 13 0
10 [VV2006] J134206.3-003702 QSO 13 42 06.3477998304 -00 37 01.231600989   20.68 20.34     ~ 11 0
11 QSO B1340+277 QSO 13 42 35.91 +27 29 11.7   21.0 21.4     ~ 6 0
12 [VV96] J134424.0-002846 QSO 13 44 23.958 -00 28 46.53   21.71       ~ 6 0
13 Feige 92 * 14 11 31.8784449873 +50 07 04.145893027   11.42 11.50     B9kp 38 0
14 2E 3238 Sy1 14 19 03.8170384929 -13 10 44.781525412   16.46 16.10 16.50   ~ 222 0
15 [VV2006] J143400.1+002648 QSO 14 34 00.0927322614 +00 26 49.100746888     20.83     ~ 11 0
16 2MASS J15315047+2423178 QSO 15 31 50.4623719187 +24 23 17.737780266   20.52   19.17   ~ 9 0
17 [VV2006] J153231.6-231032 QSO 15 32 31.5255866479 -23 10 32.439064656     21.4     ~ 10 0
18 [VV2000] J162359.1+554108 QSO 16 23 59.206 +55 41 08.78   21.02 20.79     ~ 8 1
19 [VV2000] J162421.1+554243 QSO 16 24 21.286 +55 42 43.07   21.97 21.87     ~ 8 1
20 Ross 640 WD* 16 28 25.0030292072 +36 46 15.849157470   14.01   13.9   DZA5.5 168 0
21 QSO B1634+332 QSO 16 36 21.096 +33 09 42.76   21.22 21.02     ~ 6 0
22 QSO B1640+4056 QSO 16 42 26.902 +40 50 34.34   20.4 20.4     ~ 8 0
23 SDSS J171941.24+592242.1 QSO 17 19 41.2471075333 +59 22 42.070612242   21.06 20.69     ~ 3 0
24 QSO B1721+3400 QSO 17 23 12.4819272067 +33 57 59.840642736   21.01 20.86     ~ 8 0
25 QSO B1834+509 QSO 18 36 09.2426662657 +51 00 22.252481116   20.2 20.2     ~ 6 0
26 QSO B1835+509 QSO 18 36 14.4393685836 +51 01 44.616365848   20.6 20.6     ~ 7 0
27 LAWD 73 WD* 19 00 10.2534325163 +70 39 51.418372586   13.24   13.5   DAP4.5 220 0
28 [VV2006] J205620.5-043059 QSO 20 56 20.5832359957 -04 31 00.689226746           ~ 6 0
29 [VV96] J224314.4+005528 QSO 22 43 14.2829619841 +00 55 28.207153614   20.69 20.36     ~ 9 0
30 HD 219175 PM* 23 14 07.4752698450 -08 55 27.581287520   8.12 7.56     F7V 83 0
31 [VV2006] J234752.5+010306 QSO 23 47 52.5603647706 +01 03 05.042258966           ~ 11 0

    Equat.    Gal    SGal    Ecl

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2020.07.08-03:44:42

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