Spectral Energy Distributions And Multiwavelength Selection Of Type 1 Quasars

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The XMM-Newton wide field survey in the COSMOS field

7 Max-Planck-Institut für extraterrestrische Physik, Giessenbachstrasse 1, 85748 Garching, Germany Received 31 January 2019 / Accepted 18 June 2019 ABSTRACT Aims. We study the spatial clustering of 632 (1130) XMM-COSMOS active galactic nuclei (AGNs) with known spectroscopic or

Gordon T. Richards, Publications 1997-2016

Quasar Target Selection for Data Release Nine , ApJS, 199, 3 172. Lane, R. A., et al. 2011, The Ultraviolet-to-mid-infrared Spectral Energy Distribution of

XMM#Newton Observations of the Red Type 1.8 Quasar 2M1049

Subject headinggs: quasars: individual (2MASS J1049+5837) X-rays: galaxies 1. INTRODUCTION The strong dependence of their multiwavelength appearance on the inclination to the line of sight is both a fascinating and frustrating feature of active galactic nuclei (AGNs). As a re-sult, the subset of the population being studied depends strongly

Curriculum Vitae Jonathan R. Trump

Successful Proposals (selected) - $1.5M in active grants 2020 PI, NSF CAREER: Echo Mapping the Census of Supermassive Black Hole Mass, Accretion, and Spin, $740k 2019 PI, NASA ADAP: Spectral Energy Distributions of Echo-Mapped Quasars, $540k 2018 PI, HST proposal: Ultraviolet Echoes of Quasar Accretion Disks, 40 orbits, $208k

Dr. J. Aird The demographics and evolution of AGN from

Dr. T. kawamuro Title: A Chandra and ALMA Study of X-ray-irradiated Gas in the Central ~100 pc of the Circinus Galaxy Abstract: The AGN effect on host galaxies is an interesting topic that has been often discussed so far. The AGN is usually X-ray luminous, and thus X-ray irradiation by the AGN is unavoidable for its host galaxy.


SPECTRAL ENERGY DISTRIBUTIONS AND MULTIWAVELENGTH SELECTION OF TYPE 1 QUASARS Gordon T. Richards,1,2 Mark Lacy,3 Lisa J. Storrie-Lombardi,3 Patrick B. Hall,4 S. C. Gallagher,5 Dean C. Hines,6 Xiaohui Fan,7 Casey Papovich,7 Daniel E. Vanden Berk,8 George B. Trammell,8 Donald P. Schneider,8 Marianne Vestergaard,7 Donald G. York,9,10 Sebastian Jester,11,12

X-shooting GRBs at high redshift: probing dust production

NIR spectroscopic spectral energy distributions (SEDs) provides individual extinction curves of GRB afterglows to understand dust properties at high redshifts. Previously, Zafar et al. (2011a) reported a sudden drop in dust content in GRB afterglows above z≥4 with a lack of A V ∼0.3mag extinguished events. Recently, Bolmer et al. (2018

The 1 < z < 5 Infrared Luminosity Function of Type I Quasars

define type I quasars as AGNs with optical and ul-traviolet emission lines broader than 1000 km s−1 and type II quasars as those with narrower lines. In this paper we adopt a cosmology of Ω m

Multi-Wavelength Properties of Radio-loud Narrow-Line

available Northern and Southern radio catalogues. Even though we use the term quasars, here, we generally do not distinguish between narrow-line type 1 quasars, and narrow-line Seyferts 1s, but call all sources NLS1s for the sake of brevity. The main findings can be summarized as follows: Only 7% of the NLS1 galaxies are radio-loud (R>10).

Multi-wavelength classification of unidentified AGN in the

of no or weak emission lines while quasars have strong narrow and broad emission lines. Spectral energy distributions (SEDs) of blazars are characterised by two-peaks, namely a low-energy peak extending from radio to UV/X-rays, and a high-energy peak that extends from X-rays to GeV/TeV gamma-rays.


our selection criteria (J K > 1:7, R K > 4:0) yield a 50% success rate for discovering quasars substantially redder than those found in optical surveys. Comparison with UVX- and optical color-selected samples shows that k10% of the quasars are missed in a magnitude-limited survey. Simultaneous two-frequency radio observationsfor


Quasars and Narrow-Line Seyfert Is: Trends and Selection Effects 265 Joseph C. Shields k Anca Constantin Emission and Absorption in Narrow-Line Seyfert 1 Galaxies 269 Anca Constantin k Joseph C. Shields RASS Detected Narrow-Line Seyfert 1 Galaxies in the SDSS 273 Luigi C. Gallo, Thomas Boiler, Wolfgang Voges, Scott F. Anderson,

A Search for the Smallest Supermassive Black Holes

A Search for the Smallest Supermassive Black Holes Dissertation Presented in Partial Fulfillment of the Requirements for the Degree Doctor of Philosophy

Reconciling inverse-Compton Doppler factors with

1=(4+2 ) (1 + z); (1) where F m is the synchrotron flux density of the core at frequency m and F ˜is the X-ray flux density, both in Jy; d is the angular size of the core in milliarcsec, ˜ is the X-ray observations en-ergy in keV, m is the radio observations frequency in GHz; and b is the synchrotron high-energy cutof,f which is assumed to

arXiv:1711.05476v1 [astro-ph.GA] 15 Nov 2017

Quasars (FSRQ), to check the origin for such di erent spectral properties (BLLs showing very weak or absent emission lines in the optical, instead FSRQs with promi-nent lines), as well as the distributions of the two pop-ulations in space-time and their cosmological evolution (Ghisellini et al.2017).


Type 1 AGN thanks to the HST capabilities, using either non-parametric PSF subtraction or 2-dimensional modeling (Peng et al. 2002; Jahnke et al. 2004; Sanchez et al. 2004; Peng et al. 2006).

Safeguarding & eSafety

Safeguarding & eSafety. Print Email Safeguarding at St. Joseph s. St Joseph s is a welcoming environment where everyone is highly valued and where tolerance, honesty, co-operation and mutual respect for all are fostered.

EGRET Team Papers to be Published in the Proceedings of

estimate the stellar emissivity and spectral energy distributions vs. redshift they adapted the analysis of Fall, Chariot, & Pei (1996), consistent with the Canada-France Redshift Survey. They included corrections for metallicity evolution. They found that the stellar emissivity peaks between z = 1 and 2, leading to a significant redshift-

A Pc-scale study of radio-loud AGN : The Fanaroff Riley

radio-loud quasars, FRI (and II) = Fanaroff-Riley type I (and II) radio galaxies. 3 1.2 Schematic showing the current paradigm for radio-loud AGNs. For the purpose

A multi-wavelength survey of AGN in the XMM-LSS field

Methods.The KXmethod identifies quasars on the basis of their optical (R and z ) to near-infrared (K s) photometry and point-like morphology. We combine these data with optical (u∗,g ,r ,i ,z ) and mid-infrared (3.6−24µm) wavebands to reconstruct the spectral energy distributions (SEDs) of candidate quasars.

Discovery of -ray emission from steep radio spectrum NLS1s

-ray emissions from radio galaxies as well as steep spectrum radio quasars (SSRQs), the so-called mis-aligned AGNs (MAGNs), whose jet inclination angle is larger than blazars, have been also detected (e.g. Abdo et al. 2010a). An universal two-bump structure in log F -log plot appears in their spectral energy distributions (SEDs).

Applying Relativistic Reconnection to Blazar Jets

energy, however their energy distributions are much softer than those of the electrons [16]. In the case when both electrons and ions are relativistic, they obtain similar energy distributions with hard power-law spectra [17], hence this case is qualitatively similar to reconnection in relativistic pair plasma.

A multi-wavelength survey of AGN in the XMM-LSS field: I

populations using di erent energy bands encompasses a risk of confusion between di erent types of objects or di erent physical processes. Thus, studying the selection e ects is an essential step to understanding the properties of the parent population. A classic method to identify type-1 quasars

Highlights of Recent Multiwavelength Observations of VHE

Quasars) are active galactic nuclei (AGN) with a rela-tivistic plasma jet oriented close to the line of sight [1]. These objects exhibit rapid variability and have broad-band spectral energy distributions (SEDs) characterized, in a νFν representation, by a synchrotron component extending from radio to X-ray frequencies, and a second

Properties of dusty tori in active galactic nuclei I

served spectral energy distributions (SEDs) of SDSS quasars and a precomputed grid of torus models. The observed SEDs comprise SDSS photometry, Two-Micron All-Sky Survey J, H and K data, whenever available, and mid-infrared (mid-IR) data from the Spitzer Wide-area InfraRed Extragalactic Survey. The adopted model is that of Fritz, Franceschini & Hatzim-

Submitted to the Astrophysical Journal

individual (ISS J142950.9+333012) quasars: individual (ISS J142738.5+331242) 1. Introduction Wide-area surveys are one of the most powerful tools for observational astronomy, and have led to discoveries ranging from Earth-crossing asteroids to the most distant quasars. Historically,

Joint Programs in the Context of Cross Facilities

strongly supports coronal energy and mass supply by a continuous sequence of rapid explosive energy releases. - Variable emission-line fluxes in the He-like triplets of O VII and Ne IX allow to determine density variations, implying densities between 2×10. 10 and 4×1011 cm-3 Estimates of the mass and the volume of the line-emitting plasma.

Curriculum Vitae - Bangalore University

Spectroscopic Study of Seyfert 1 galaxies and quasars submitted to Bangalore University, Bangalore, Karnataka State, India 3. Positions held in the University: 1. Lecturer, November 24, 1992 2. Lecturer (Senior Scale), November 24, 1997 3. Lecturer (Selection Grade), November 24. 2002 4. Reader, August 8, 2005 5. Associate Professor, January 1, 2006

Statistical multifrequency study of narrow-line Seyfert 1

The spectral energy distributions (SEDs) of some radio-loud NLS1 sources are similar to the SEDs of blazars. In them the most prominent features are two broad components, one ex-tending from radio to soft X-rays and the other covering hard X-rays and -rays. The first bump is believed to be due to syn-


Received 2008 May 15; accepted 2008 August 25; published 2008 December 1 ABSTRACT We study the spectral energy distributions and evolution of a large sample of optically selected quasars from the Sloan Digital Sky Survey that were observed in 323 Chandra images analyzed by

Chalmers Publication Library

by adopting an observed AGN spectral index Γ obs = 1.4 (e.g., Xue et al. 2011). The L 2−10keV of our sample have a range from ∼3 ×1043 erg s−1 to 1045 erg s−1 with a median value of 1.5 × 1044 erg s−1, about one order of magnitude higher than the previous moderate-luminosity sample in a similar redshift

2007 Aug Hines bibliography

22. Richards, G.T. et al. 2006, ApJS, Spectral Energy Distributions and Multiwavelength Selection of Type 1 Quasars, 166, 470 23. Schneider, G., et al. 2006, Discovery of an 86 AU Radius Debris Ring Around HD 181327, ApJ, 650, 414 24. Smith, P.S., et al. 2006, Spitzer Far-Infrared Detections of Cold Circumstellar Disks, 644, L125 25.

A Complete Multiwavelength Characterization of Faint

We have constructed spectral energy distributions (SEDs) for each source using datafromthefourIRACwavebands,Chandrafluxesinthehard(2 8keV)andsoft(0.5 2keV)X-rays,andoptical follow-updatainthewavebandsU,g 0 ,r 0 ,i ,Z,andH.WefitanumberofspectraltemplatestotheSEDsatopticaland


of the properties of binary quasars such as their environments, spectral energy distributions (SEDs), and nuclear and host galaxy properties provide useful information to help distinguish which systems may be undergoing merging or triggering, and to elucidate merger physics itself. In this paper, we probe the multiwavelength properties of

Telescopes at Kitt Peak National Observatoryg

PUBLICATIONS USING DATA FROM NOAO TELESCOPES Telescopes at Kitt Peak National Observatory. g. Aga. fonov, M., Richards, M., Sharova, O. 2006, ApJ, 652, 1547, Three

Spectroscopy Science Cases and Capability Needs: Galaxies

emission or Ly break energy distributions can provide a high density of probes for the 3-D structure of inflowing and outflowing gas, as well as its association with individual objects. Need 10-arcmin FOV, MOS coverage of i-25.5 with S/ N~10, 100s of objects, accurate RV s, R~2000, coverage 0.4-1.0um for rest-frame UV coverage 2

Searching for new TeV blazars in the 3rd Fermi-LAT

The Spectral Energy Distributions (SEDs) of AGN display a double humped shape consisting of a low energy component extending from radio to X-ray energies and a High Energy (HE) component that can extend from X-ray up to TeV energies. The low energy emission is considered to be synchrotron emission from a population of relativistic

Conference Highlights - JSTOR

The spectral energy distributions (SEDs) of blazars were interpreted as a combination of synchrotron emission and higher energy radiation, possibly from Compton scattering. The observed SEDs follow an interesting trend with lumi-nosity, such that high-luminosity blazars have synchrotron and Compton peaks at lower frequencies. This can be

Constraining the Evolutionary Stage of Class I Protostars

04381+2540, 1.3 mm data were also obtained with the high configuration, which provides baselines from 35 to 240 m. Continuum data were recorded in four 1-GHz channels. We calibrated the amplitudes and phases of the data using quasars near on the sky (. 20 ) to our target sources.


otherwise. We use the terms type 1 and type 2 for AGNs with broad and narrow optical emission lines, respectively, in their optical spectra. We introduce a new nomenclature for the broadband SED classification: AGN1, AGN2, and SF. The term AGN1 refers to an SED that is fitted by a type 1

Abstract Booklet - ESO

quasars. Using a combination of mid-infrared and radio data (from Spitzer and the VLA) we have found a successful method of finding for z>∼2 type-2 quasars. These obscured quasars probably outnumber the unobscured (type-1) quasars by a ratio ∼2-3:1. I will discuss

Spectral Energy Distributions of Quasars and AGN

Spectral Energy Distributions of Quasars and AGN Belinda J. Wilkes Smithsonian Astrophysical Observatory, 60 Garden St., Cambridge MA 02138, USA Abstract. Active Galactic Nuclei (AGN) are multiwavelength emitters. To have any hope of understanding them, or even to determine their energy output, we must observe them with many telescopes. I will review

Search for High-Confidence Blazar Candidates and Their MWL

Quasars (FSRQs) in the 2FGL catalog, and Doert and Errando [5] classified AGN and non-AGN with a combination of random forests and neural networks. The extension to multiwavelength information especially the relation between properties extracted from different parts of the energy spectrum provides additional source type-specific

arXiv:1109.1278v1 [astro-ph.CO] 6 Sep 2011

properties of binary quasars such as their environments, spectral energy distributions (SEDs), and nuclear and host galaxy properties provide useful information to help distinguish which systems may be undergoing merging or triggering, and to elucidate merger physics itself. In this paper, we probe the multiwavelength proper-

Gordon T. Richards, Publications 1997-2017

Quasar Target Selection for Data Release Nine , ApJS, 199, 3 172. Lane, R. A., et al. 2011, The Ultraviolet-to-mid-infrared Spectral Energy Distribution of

AGN physics in the age of Fermi

Selection biases from 2 Jy FSRQs (Wall & Peacock catalog), 1 Jy BL Lac (radio selected), Spectral Energy Distributions of Blazars: Two Component Paradigm Mrk 501, z = 0.033 PG 1553+113, z < 0.75 Multiwavelength quasi-simultaneous SEDs including

Spectral models for low-luminosity active galactic nuclei

Regarding the broad-band spectral energy distributions (SEDs), LLAGNs do not seem to have the thermal continuum prominence in the ultraviolet multiwavelength observations of black hole systems and comparing we carefully applied the following selection criteria. (1)