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J/MNRAS/458/2       Gravitationally lensed quasars                 (Rusu+, 2016)

Subaru Telescope adaptive optics observations of gravitationally lensed quasars in the Sloan Digital Sky Survey. Rusu C.E., Oguri M., Minowa Y., Iye M., Inada N., Oya S., Kayo I., Hayano Y., Hattori M., Saito Y., Ito M., Pyo T.-S., Terada H., Takami H., Watanabe M. <Mon. Not. R. Astron. Soc., 458, 2-55 (2016)> =2016MNRAS.458....2R (SIMBAD/NED BibCode)
ADC_Keywords: Gravitational lensing ; QSOs Keywords: gravitational lensing: strong - instrumentation: adaptive optics - methods: data analysis - quasars: supermassive black holes - dark matter Abstract: We present the results of an imaging observation campaign conducted with the Subaru Telescope adaptive optics system (IRCS+AO188) on 28 gravitationally lensed quasars and candidates (23 doubles, 1 quad, 1 possible triple, and 3 candidates) from the SDSS Quasar Lens Search. We develop a novel modelling technique that fits analytical and hybrid point spread functions (PSFs), while simultaneously measuring the relative astrometry, photometry, as well as the lens galaxy morphology. We account for systematics by simulating the observed systems using separately observed PSF stars. The measured relative astrometry is comparable with that typically achieved with the Hubble Space Telescope, even after marginalizing over the PSF uncertainty. We model for the first time the quasar host galaxies in five systems, without a priori knowledge of the PSF, and show that their luminosities follow the known correlation with the mass of the supermassive black hole. For each system, we obtain mass models far more accurate than those previously published from low-resolution data, and we show that in our sample of lensing galaxies the observed light profile is more elliptical than the mass, for ellipticity ≳0.25. We also identify eight doubles for which the sources of external and internal shear are more reliably separated, and should therefore be prioritized in monitoring campaigns aimed at measuring time delays in order to infer the Hubble constant. Description: We described the results of a large imaging campaign with the Subaru Telescope AO, aimed at obtaining high-resolution observations of gravitationally lensed quasars from SQLS. The observations were performed between 2011 and 2014. 28 objects were successfully observed. File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 71 35 Summary of observations table3a.dat 57 22 *Information on lens systems table3.dat 100 98 Relative astrometry and photometry of the lens systems table4.dat 74 50 Morphological parameters table6.dat 82 9 Quasar host galaxy properties tablea1.dat 83 47 TT and PSF stars tablea2.dat 73 43 Analytical parameters for all best-fitted object and star PSFs, determined with hostlens table2.dat 194 30 Technique of morphology fitting
Note on table3a.dat: The results for SDSS J1405+0959, presented in a separate publication, are not included (see Appendix B19).
Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name Object name (SDSS JHHMM+DDMM) 16 A1 --- n_Name [d] Note on Name (1) 18- 23 A6 --- GStar Guide star 25- 30 A6 s ExpTime Exposure time (NNxNNN) (2) 32- 33 A2 --- Filt Filter 35- 36 I2 mas PixScale Pixel scale 38- 46 A9 --- Airmass Airmass 48- 53 A6 --- Cal Photometric calibration 54 A1 --- n_Cal [abcef] Note on Cal (1) 56- 71 A16 --- Obs.date Observation date (UTC)
Note (1): Notes as follows: a = Based on 1 star in the FOV b = based on 3 stars in the FOV c = based on 1 star and 1 galaxy in the FOV d = refers to SDSS J092634.56+305945.9 e = dark sky pattern may affect model photometry f = compared the total magnitude with the measurement in 2MASS Note (2): Exposure times show the number of frames that were combined in the final science frame.
Byte-by-byte Description of file: table3a.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name Name 16 A1 --- n_Name [g] Note on Name (1) 18- 26 A9 --- Param Parameter (theta or max.sep.) 27- 31 F5.3 arcsec Value Parameter value 33- 38 F6.4 arcsec e_Value rms uncertainty on Value 39 A1 --- n_Value [b] Note on Value (1) 41- 45 F5.3 --- zs Redshift of the source quasar 47 A1 --- l_zl [~] Limit flag on zl 48- 52 F5.3 --- zl Redshift of the main lens galaxy (2) 53 A1 --- --- [-] 54- 56 F3.1 --- zlu ? Upper value of zl interval 57 A1 --- n_zl [cehb] Note on zl (1)
Note (1): Notes as follows: b = The zero-point error is 0.14mag for both SDSS J0820+0812 and SDSS J1620+1203 c = In addition to the quoted errors on photometry, a systematic error of 0.05mag was obtained during simulations, which should be added to the absolute photometry, but does not affect the relative values e = The astrometry for SDSS J1206+4332 should be considered less reliable (see Appendix B10) g = The astrometry represents the average over the H and K" bands, and the magnitudes of G1 and G2 were obtained from aperture photometry h = Absolute photometry is unreliable due to non-photometric conditions Note (2): where zl is approximate, its value is a photometric redshift estimate.
Byte-by-byte Description of file: table3.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name SDSS name 17- 23 A7 --- Object Object 24 A1 --- n_Object [d] Note on Object (1) 25 A1 --- l_DX [~] Limit flag on DX 26- 32 F7.3 arcsec DX Offset in X direction (positive to west) 34- 39 F6.4 arcsec e_DX ? rms uncertainty on DX (2) 40 A1 --- n_DX (]) 41 A1 --- l_DY [~] Limit flag on DY 42- 48 F7.3 arcsec DY Offset in Y direction (positive to north) 50- 55 F6.4 arcsec e_DY ? rms uncertainty on DY (2) 56 A1 --- n_DY (]) 57- 61 F5.2 mag K'mag ? K' magnitude (Vega) (3) 63- 66 F4.2 mag e_K'mag ? rms uncertainty on K'mag 67 A1 --- n_K'mag [ad] Note on K'mag 69- 73 F5.2 mag K'4mag ? K' (Sersic index = 4) magnitude (Vega) (3) 75- 78 F4.2 mag e_K'4mag ? rms uncertainty on K'4mag 79 A1 --- n_K'4mag [f] Note on K'4mag 80- 84 F5.2 mag Jmag ? J magnitude (Vega) (3) 86- 89 F4.2 mag e_Jmag ? rms uncertainty on Jmag 91- 95 F5.2 mag Hmag ? H magnitude (Vega) (3) 97-100 F4.2 mag e_Hmag ? rms uncertainty on Hmag
Note (1): Notes as follows: a = The fluxes are estimated with hostlens for the point source, and reflect the uncertainty in the host galaxy-quasar disentangling, therefore attached errors should not be used to estimate the error on the flux ratio, which are smaller. d = Aperture photometry is given, and the positions and their errors are measured with the iraf PHOT task. f = Sersic index of G1a (not G1b) is fixed at 4. Note (2): The error bars on the astrometry do not include the systematic errors in Table A3. The objects without attached error bars on the positions are located at a relatively large distance from the target, where the residual distortion is expected to be large. Note (3): Magnitudes are in the Vega system. All magnitudes are corrected for atmospheric and Galactic extinction. For the objects where the quasar host galaxy has been explicitly modelled, relative photometry of the images includes the contribution of the point source as well as the host.
Byte-by-byte Description of file: table4.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name SDSS name 17- 19 A3 --- Object Object 20- 29 A10 --- Note Note 30- 33 F4.2 --- e ? Ellipticity 35- 38 F4.2 --- e_e ? rms uncertainty on e 39 A1 --- n_e [uf] u for Unreliable, f for fixed 41- 46 F6.2 deg PA []?=- Position angle (is positive from north towards east) 48- 52 F5.2 deg e_PA ? rms uncertainty on PA 54- 57 F4.2 arcsec re Effective radius 59- 62 F4.2 arcsec e_re rms uncertainty on Re 64 A1 --- l_n [~] Limit flag on n 65- 68 F4.2 --- n Sersic number 70- 73 F4.2 --- e_n ? rms uncertainty on n 74 A1 --- n_n [f] f for fixed
Byte-by-byte Description of file: table6.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name SDSS name 17- 18 A2 --- l_K'magH [≳] Limit flag on K'magH 19- 23 F5.2 mag K'magH Host K' magnitude 25- 28 F4.2 mag e_K'magH ? rms uncertainty on K'magH 30 A1 --- l_K'magN [~] Limit flag on K'magn 31- 35 F5.2 mag K'magN Nucleus K' magnitude 37- 40 F4.2 mag e_K'magN ? rms uncertainty on K'magn (1) 42 A1 --- l_e [~] Limit flag on e 43- 46 F4.2 --- e Ellipticity of the host 48- 51 F4.2 --- e_e ? rms uncertainty on e (1) 53- 56 F4.2 arcsec Reff ?=- Effective radius in arcsec 58- 61 F4.2 arcsec e_Reff ? rms uncertainty on Reff 63 A1 --- l_Reffk [~] Limit flag on Reffk 64- 66 F3.1 kpc Reffk ?=- Effective radius in kpc 68- 71 F4.2 --- n ?=- Sersic index 73- 76 F4.2 --- e_n ? rms uncertainty on n (1) 77 A1 ---- n_n [f] f for fixed Sersic index 79- 82 F4.2 --- Host/QSO Flux ratio in the source plane
Note (1): Error bars include those resulting from the simulations with a real PSF and noise, but not from the uncertainty in the radial slope of the lens mass profile.
Byte-by-byte Description of file: tablea1.dat
Bytes Format Units Label Explanations
1- 4 A4 --- --- [SDSS] 6- 25 A20 --- SDSS SDSS name (JHHMMSS.ss+DDMMSS.ss) 27- 45 A19 --- OName Description (TT or PSF or TT (PSF) JHHMM+DDMM) 47 A1 --- Band [KR] Band 49 A1 --- --- [=] 51- 55 F5.2 mag mag Magnitude in Band (from NOMAD catalog, Cat. I/297) 57 A1 --- l_Sep [~] Limit flag on Sep 58- 61 F4.1 arcsec Sep ? Separation (1) 62 A1 --- --- [;] 64- 67 F4.1 arcsec Sep2 ? Second separation value 69- 83 A15 --- Name SDSS name has in the other tables
Note (1): Separation specifies the distance between the TT star and the object, and between the TT and the PSF star, respectively.
Byte-by-byte Description of file: tablea2.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name SDSS name 17- 22 A6 --- Code Technique of morphology fitting code described in table2.dat 24- 27 F4.2 arcsec FWHM1 Core profile FWHM (1) 29- 32 F4.2 --- e1 Core ellipticity (1) 34- 38 F5.1 deg PA1 [] Core position angle (positive from north towards east) (1) 40- 44 F5.1 --- beta1 Core beta parameter (1) 45 A1 --- n_beta1 [f] f for fixed 47- 50 F4.2 arcsec FWHM2 ?=- Wings profile FWHM (1) 52- 55 F4.2 --- e2 ?=- Wings ellipticity (1) 57- 61 F5.1 deg PA2 []?=- Wings position angle (positive from north towards east) (1) 63- 65 F3.1 --- beta2 ?=- Wings beta parameter (1) 67- 70 F4.2 --- F1/(F1+F2) ?=- Total to core flux ratio 72- 73 I2 % Strehl ?=- Strehl ratios were computed by comparing the peak flux of the PSF with that of a diffraction-limited PSF model
Note (1): The fitting was performed on the co-added, final frames. Affix 1 refers to the core, and affix 2 refers to the wings, both modelled as Moffat profiles.
Byte-by-byte Description of file: table2.dat
Bytes Format Units Label Explanations
1- 15 A15 --- Name Object name (SDSS JHHMM+DDMM) 17- 24 A8 --- Code Technique of morphology fitting code 26-194 A169 --- Tech Technique of morphology fitting
History: From electronic version of the journal
(End) Patricia Vannier [CDS] 25-Nov-2016
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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