[PDF] Top 20 Revealing a population of heavily obscured active galactic nuclei at z approximate to 0 5 1 in the chandra deep field south

... required to cal- culate the IR-based and UV-based SFRs in the ISX ...method. The CDF-S and E-CDF-S have been covered by extensive photometric and spectroscopic surveys, and we ... See full document

... for the sources in the sample are in the range of ...chose the extraction radius for each source to obtain an acceptable trade-off between the number ... See full document

... total of 343 (81.9%) of the 419 spectroscopic redshift measure- ments are “secure,” in that they are measured at 95% confi- dence levels with multiple secure spectral ...|Δ z | ... See full document

... for the recently completed ≈4 Ms Chandra Deep Field-South (CDF-S) survey, the deepest X-ray survey to ...calculation of number counts down to flux limits ... See full document

... all of the spectra are combined and binned to increase the signal-to-noise ...ratio. The composite X-ray spectrum of the heavily obscured AGNs is ... See full document

... from the MUSYC medium-band survey in the Extended Chandra Deep Field-South (ECDF-S), we fit synthetic stellar population models to compare active ... See full document

... for the 462 X-ray sources in the ≈2 Ms Chandra Deep Field-South (CDF-S) ...using deep optical-to-radio multiwavelength catalogs, and are then combined ... See full document

... advantage of the rich multiwavelength data available in the Chandra Deep Field South (CDF-S), including the 4 Ms Chandra observations (the ... See full document

... present the fi rst direct measurements of the rest-frame 10 – 40 keV X-ray luminosity function ( XLF ) of active galactic nuclei ( AGNs ) based on a sample of 94 ... See full document

... wavdetect at a false-positive probability threshold of 10 − 5 in at least one of three X-ray bands ...criterion of P < 0.004 (i.e., the probability of ... See full document

... variety of source types; 55% of them appear to be active galactic nuclei, while 45% appear to be starburst and normal ...galaxies. In addition to the ... See full document

... Most of our objects lie below λ ∼ 0.1 which means that the range of high Eddington ratios is not fully probed by the CDF ...AGN. To sample the area of λ & 0.1 requires ... See full document

... used to arrive at a new level 2 event file. Before applying the new CIAO tool to identify ACIS hot pixels and cosmic-ray afterglow events, the pixels identified in the ... See full document

... by Chandra has an angular size of ∼ 12 arcsec, which at the distance of the source corresponds to ∼ ...related to thermal plasma in a star-forming region, ... See full document

... caveat of most studies of star-formation in AGN hosts is that they tend to concentrate on low and moderate luminosity ...because the emission of the active nucleus ... See full document

... and deep SCUBA2 Cosmology Legacy Surveys will provide larger samples of SMGs with which to test these results and provide further insight into the relationship be- tween the growth ... See full document

... arguments to estimate how many SMGs are still unaccounted for, and thus likely undetected in our optical and mid-IR ...out of the sample of 126 LESS SMGs without robust radio, 24- µ m ... See full document

... for the specific structure, geometry, and composition of the obscuring material surround- ing the central supermassive black hole (SMBH): (1) a uniform (smooth/continuous), ... See full document

... detections in the UKIDSS K and WISE W1 bands (black circles), with different classes highlighted by the colors as indicated in the legend: the R - W1 ( Vega ) diagnostic is well ... See full document

... with the derivation of the physical properties of 37 Balmer break galaxies, which have the necessary lines to locate them in star-forming–active galactic ... See full document