2013A&A...556A..97C


C.D.S. - SIMBAD4 rel 1.7 - 2019.11.13CET12:01:27

2013A&A...556A..97C - Astronomy and Astrophysics, volume 556A, 97-97 (2013/8-1)

Towards equation of state of dark energy from quasar monitoring: reverberation strategy.

CZERNY B., HRYNIEWICZ K., MAITY I., SCHWARZENBERG-CZERNY A., ZYCKI P.T. and BILICKI M.

Abstract (from CDS):

High-redshift quasars can be used to constrain the equation of state of dark energy. They can serve as a complementary tool to supernovae Type Ia, especially at z>1. The method is based on the determination of the size of the broad line region (BLR) from the emission line delay, the determination of the absolute monochromatic luminosity either from the observed statistical relation or from a model of the formation of the BLR, and the determination of the observed monochromatic flux from photometry. This allows the luminosity distance to a quasar to be obtained, independently from its redshift. The accuracy of the measurements is, however, a key issue. We modeled the expected accuracy of the measurements by creating artificial quasar monochromatic lightcurves and responses from the BLR under various assumptions about the variability of a quasar, BLR extension, distribution of the measurements in time, accuracy of the measurements, and the intrinsic line variability. We show that the five-year monitoring of a single quasar based on the Mg II line should give an accuracy of 0.06-0.32mag in the distance modulus which will allow new constraints to be put on the expansion rate of the Universe at high redshifts. Successful monitoring of higher redshift quasars based on C IV lines requires proper selection of the objects to avoid sources with much higher levels of the intrinsic variability of C IV compared to Mg

Abstract Copyright:

Journal keyword(s): quasars: emission lines - cosmological parameters - dark energy - accretion, accretion disks - black hole physics

Simbad objects: 17

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Number of rows : 17

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 1501 Sy1 00 10 31.0058529490 +10 58 29.505989476   15.96 15.40 12.22   ~ 625 0
2 Mrk 1502 Sy1 00 53 34.9326560879 +12 41 35.927159668   14.41 14.03     ~ 1008 1
3 ESO 113-45 Sy1 01 23 45.7630391439 -58 48 20.811630442   14.08 13.83 13.34   ~ 745 0
4 [VV2006] J052247.2-710130 QSO 05 22 47.1936739105 -71 01 30.836487265     19.44   18.57 ~ 13 0
5 QSO B0636+68 QSO 06 42 04.2571549110 +67 58 35.621670643     16.46 16.01   ~ 198 1
6 7C 083620.60+710405.00 QSO 08 41 24.36526906 +70 53 42.1730054     16.5 16.8   ~ 681 1
7 6C 111613+602056 QSO 11 19 14.3457832564 +60 04 57.203550711   17.60 17.38 16.9   ~ 58 1
8 QSO J1120+0641 QSO 11 20 01.48 +06 41 24.3           ~ 152 0
9 QSO B1125-1302 QSO 11 28 18.5903860431 -13 19 28.724738443     16.61     ~ 17 0
10 NGC 3783 Sy1 11 39 01.7095761008 -37 44 19.008597647   12.46 13.43 11.33 12.1 ~ 1445 0
11 NGC 4151 Sy1 12 10 32.5771747733 +39 24 21.057727323   12.18 11.48     ~ 3308 2
12 [VV96] J123549.4+591028 QSO 12 35 49.4624610031 +59 10 27.061004102   17.41 17.21     ~ 32 0
13 NGC 5548 Sy1 14 17 59.5401093128 +25 08 12.600227883   14.35 13.73     ~ 2336 0
14 QSO B1425+606 QSO 14 26 56.1848058014 +60 25 50.814100630   16.82 16.54     ~ 117 0
15 HS 1700+6416 QSO 17 01 00.6195618802 +64 12 09.118927057   16.39 16.17     ~ 328 0
16 ICRF J184208.9+794617 Sy1 18 42 08.9910523393 +79 46 17.129210139   16.06 15.38     ~ 1188 0
17 LBQS 2113-4538 QSO 21 16 44.3147551838 -45 26 10.223233009     17.3     ~ 15 0

    Equat.    Gal    SGal    Ecl

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2019.11.13-12:01:27

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