* Your assessment is very important for improving the workof artificial intelligence, which forms the content of this project
Download Y-band Imaging of Extragalatic Fields and High redshift
Wilkinson Microwave Anisotropy Probe wikipedia , lookup
James Webb Space Telescope wikipedia , lookup
International Year of Astronomy wikipedia , lookup
Spitzer Space Telescope wikipedia , lookup
History of the telescope wikipedia , lookup
History of gamma-ray burst research wikipedia , lookup
Astronomy in the medieval Islamic world wikipedia , lookup
Astronomical seeing wikipedia , lookup
Star formation wikipedia , lookup
History of astronomy wikipedia , lookup
Cosmic distance ladder wikipedia , lookup
Timeline of astronomy wikipedia , lookup
Brown dwarf wikipedia , lookup
Theoretical astronomy wikipedia , lookup
Leibniz Institute for Astrophysics Potsdam wikipedia , lookup
Hubble Deep Field wikipedia , lookup
International Ultraviolet Explorer wikipedia , lookup
Y-band Imaging of Extragalatic Fields and High redshift Quasars Changsu Choi1, Myungshin Im1 1Center for the Exploration of the Origin of the Universe, Astronomy Program, Department of Physics and Astronomy, Seoul National University Abstract We carried out the observations of several extragalactic fields, brown dwarfs, high-z QSO and A0V standard star imaging with Y-band filter at the Mt. Lemmon Opti cal Astronomy Observatory (LOAO) and the Maidanak Observatory. The deepest limit magnitude of 260 minutes exposure is Y = 21.5 AB mag in case of LOAO and Y = 22 AB mag for the Maidanak Observatory. Using the Y-band imaging data, we measured photometric calibration parameters of Y-band. We got two photometric calibration parameters atmospheric extinction coefficient k = 0.087 and zero point ξ = 18.29 in LOAO , k = 0.1 and zero point ξ = 19.14 mag in Maidanak Obser vatory. We performed number counts in Y-band imaging fields and found slopes consistent with previous I-band and J-band data. Also, we tested the usefulness of hig h redshift QSO (z > 6) selection via i-z VS z-Y color-color diagram. The discrimination method between them with i-z va z-Y color-color diagram shows that it is as effective as the i-Y vsY-J color-color diagram method which means we can search high redshift QSOs effectively with an optical CCD installed at 1m class telescopes . Furthermore we analyzed characteristics of Y-band objects with color-magnitude diagram and redshift -Y-band magnitude relation. Introduction Results Y-band is emerging as a key filter of recent observations for its unique wavelength regi on. But Past work with Y-band is still few an d restricted stellar objects. It is good for id entification of low mass stars and brown d warf. (Hillenbrand et al. 2002) Extragalactic study with Y-band is very imp ortant tool for high redshift objects. The m ost highlighted aspect is High-z QSOs(z >6 ) photometric selection method (Fan et al. 2000,2001; Warren & Hewett et al. 2002). So Y-band is adopted to UKIDSS, Pan-STAR RS on that purpose. We performed Deep Y-bang imaging of extr agalactic fields with optical CCD at 1-m cla ss telescope with these goals. 1. Y-band transmission curve. Green line is z~7 QSO SED and red line is L dwarf SED. High-z QSO selection with color-color diagram Venemans et al.(2007) high-z QSOs(black) is seperated from dwarf stars(yellow) • 1 mag deeper than UKIDSS (20.4 AB mag) and ah ead of Pan-STARRS • 2.Provide Photometric calibration data • 3. Number count of detected sources for first time in Y-band • 4.Color-color diagram : high-z QSO selection met hod Here we present two results from our study. 1. Number count of our total observed field 2. Color-color Diagram of i-z vs z-Y 1.Number count Bright end : stellar sources Faint end : extended sources(extragalactic) Number count shows intermediate feature between I and J-band number count Black circle is total objects and blue square is stellar objects. Data . Summary of observations Log (Exp.time ) Area (deg2) Depth 5σ (AB mag) EGS 4.18 0.1 20.2 FLS 3.7 0.1 20.0 NEP 2.95~4.2 0.96 18.4~20.5 UKIDSS 3.4 0.1 19.2 # CFHT LS W1 3.75, 3.8 0.2 21.3 # NEP 3.9 0.2 21 #GRB090429B 4.0 0.1 21.8 *SDSS J113717+354956.9 3.4 0.1 19.2 *SDSS J084035+562419.9 3.7 0.1 19.8 *SDSS J084119+290504.4 3.65 0.1 19.7 *SDSS J092721+200123.7 3,7 0.1 19.6 *SDSS J125051+313021.9 3.7 0.1 19.6 SDSS J065405+652805.4 3.6 0.1 19.6 SDSS J083506+195304.3 3.5 0.1 19.1 SDSS J104335+121314.1 3.5 0.1 19.5 SDSS J121951+312849.4 3.5 0.1 19.0 SDSS J090900+652527.1 3.4 0.1 19.0 Target We observed total 2 square deg using LOAO 1m, Maidanak 1.5m telescope (#) Observed targets are famous extragalactic fields, 5 brown dwarf,(*) and 5 SDSS QSOs (z~6). Details are on the table left. We used IRAF tasks for Pre-process and image stacking. SCAMP and SWARP is used for astrometry. Reference catalog is USNO B-1 catalog, its matching rms ~ 1” A0V stars from HIPPARCOS catalog were observed for standard star, which have zero color. From that we calculated atmospheric extinction coefficeint k = 0.05 ~ 0.1 We performed photometry using Source Extractor and cross-matched with SDSS DR7, CFHT LS T0003, UKIDSS DR2 plus, CFHT-NEP matched catalog, DEEP2 redshift catalog 2. Color-Color Diagram i-z vs z-Y Red line is SF galaxy evolution and blue line represents QSOs as z goes higher In this figure, we can verify that i-z vs z-Y color is effective method for high –z QSO(stars) distinction from L,T dwarfs(squares). Black dot are observed Y-band source. But we could not find high-z QSO candidate from our observation. Discussion & Future works We archived depth of 21mag with 2hr exposure with 1-m class telescopes. It shows potential of 1-m class telescopes with unique and elaborated effort. In right figure, Sensitivity limit of LOAO versus Maidanak is shown. The difference is about 1mag. Red arrow indicates 1mag improved depth with refined mirror. Green arrow indicate z-band depth of 60min exposure. Other application of Y-band imaging is GRB afterglow observation. We carried out deep Y-band imaging observation at LOAO & Maidanak . We try to search high-z QSOs with this method with wider and deeper observations. Summary We observed 2 sq deg extragalactic fields, 5 QSOs and 5 dwarfs with Y-band filter. We performed Y-band source number count and inspect Y-band sources. We found i-z VS z-Y color-color diagram is effective method of high-z QSO photometric selection. There are another potentialities of 1m class telescope and Y-band observation. We try to search high-z QSOs(z>6) with this method and related works is undergoing. Email:[email protected]