Arash Bodaghee - Georgia College

Arash Bodaghee
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Arash Bodaghee
Georgia College
United States

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High Energy Astrophysical Phenomena (30)
Solar and Stellar Astrophysics (2)
Astrophysics of Galaxies (2)
Astrophysics (1)
Instrumentation and Methods for Astrophysics (1)

Publications Authored By Arash Bodaghee

Affiliations: 1Remeis-Observatory and ECAP, FAU Erlangen, 2Remeis-Observatory and ECAP, FAU Erlangen, 3Remeis-Observatory and ECAP, FAU Erlangen, 4MIT Kavli Institute, 5CRESST-UMBC, 6MIT Kavli Institute, 7Remeis-Observatory and ECAP, FAU Erlangen, 8Remeis-Observatory and ECAP, FAU Erlangen, 9IMAPP, Radboud-University Nijmegen, 10IoA, University of Cambridge, 11CEA Saclay, 12Max Planck Computing and Data Facility, 13Dept. of Chemistry, Physics, and Astronomy, Georgia College and State University, 14SSL UC Berkeley, 15Harvard John A. Paulson School of Engineering and Applied Sciences and CfA, 16LLNL, 17Remeis-Observatory and ECAP, FAU Erlangen

The accretion onto the black hole in the system HDE 226868/Cygnus X-1 is powered by the strong line driven stellar wind of the O-type donor star. We study the X-ray properties of the stellar wind in the hard state of Cyg X-1 as determined with data from the Chandra High Energy Transmission Gratings. Large density and temperature inhomogeneities are present in the wind, with a fraction of the wind consisting of clumps of matter with higher density and lower temperature embedded in a photoionized gas. Read More

Affiliations: 1Georgia College, 2SSL-UC Berkeley, 3SSL-UC Berkeley, 4IKI Moscow, 5JPL-Caltech, 6Columbia University, 7ESO, 8SSL-UC Berkeley, 9DTU Space, 10SSL-UC Berkeley, 11Columbia University, 12Caltech, 13NASA-GSFC

The high-mass X-ray binary and accreting X-ray pulsar IGR J16393-4643 was observed by NuSTAR in the 3-79 keV energy band for a net exposure time of 50 ks. We present the results of this observation which enabled the discovery of a cyclotron resonant scattering feature with a centroid energy of 29.3(+1. Read More

Affiliations: 1Remeis Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany, 2Remeis Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany, 3MIT-Kavli, 4Remeis Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany, 5CEA DSM/IRFU/SAp, Centre de Saclay, France, 6SSL, University of California Berkeley, 7Remeis Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany, 8CRESST and NASA GSFC, 9MIT-Kavli, 10Remeis Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany, 11MPCDF, Garching, Germany, 12SSL, University of California Berkeley, 13IoA, Cambridge, UK, 14Department of Astronomy and Maryland Astronomy Center for Theory and Computation, UMD, 15IAAT, Tübingen, Germany, 16ESA-ESOC Darmstadt, Germany, 17IAAT, Tübingen, Germany, 18Remeis Sternwarte and ECAP, Universität Erlangen-Nürnberg, Germany

We report on the analysis of the broad Fe Kalpha line feature of Cygnus X-1 in the spectra of four simultaneous hard intermediate state observations made with the X-ray Multiple Mirror mission (XMM-Newton), the Rossi X-ray Timing Explorer (RXTE), and the International Gamma-Ray Astrophysics Laboratory (INTEGRAL). The high quality of the XMM-Newton data taken in the Modified Timing Mode of the EPIC-pn camera provides a great opportunity to investigate the broadened Fe Kalpha reflection line at 6.4keV with a very high signal to noise ratio. Read More

Affiliations: 1SSL/UCB, 2Space Research Institute, 3SSL/UCB and HKU, 4Georgia College, 5AIM and Institut Universitaire de France, 6ESO and Harvard, 7AIM, 8SSL/UCB and UCB

We report on 0.3-10 keV observations with the Chandra X-ray Observatory of eight hard X-ray sources discovered within 8 degrees of the Galactic plane by the INTEGRAL satellite. The short (5 ks) Chandra observations of the IGR source fields have yielded very likely identifications of X-ray counterparts for three of the IGR sources: IGR J14091-6108, IGR J18088-2741, and IGR J18381-0924. Read More

Affiliations: 1Washington University in Saint Louis, Physics Department and McDonnell Center for the Space Sciences, 2Jet Propulsion Laboratory, 3California Institute of Technology, Cahill Center for Astronomy and Astrophysics, 4Washington University in Saint Louis, Physics Department and McDonnell Center for the Space Sciences, 5Washington University in Saint Louis, Physics Department and McDonnell Center for the Space Sciences, 6Washington University in Saint Louis, Physics Department and McDonnell Center for the Space Sciences, 7Washington University in Saint Louis, Physics Department and McDonnell Center for the Space Sciences, 8Washington University in Saint Louis, Physics Department and McDonnell Center for the Space Sciences, 9Washington University in Saint Louis, Physics Department and McDonnell Center for the Space Sciences, 10Anton Pannekoek Institute for Astronomy, 11California Institute of Technology, Cahill Center for Astronomy and Astrophysics, 12California Institute of Technology, Cahill Center for Astronomy and Astrophysics, 13Jet Propulsion Laboratory, 14Jet Propulsion Laboratory, 15Rice University, Department of Physics and Astronomy, 16Washington University in Saint Louis, Physics Department and McDonnell Center for the Space Sciences, 17Georgia College, Department of Chemistry, Physics, and Astronomy, 18Jet Propulsion Laboratory, 19Jet Propulsion Laboratory, 20North-West University, Centre for Space Research, 21Technical University of Denmark, DTU Space, National Space Institute, 22Yale University, Department of Astronomy, 23Washington University in Saint Louis, Physics Department and McDonnell Center for the Space Sciences, 24University of Virginia, Department of Astronomy, 25MPI for Extraterrestrial Physics Garching, 26Durham University, Centre for Extragalactic Astronomy, Department of Physics, 27Jet Propulsion Laboratory, 28North Carolina State University, Department of Physics, 29Jet Propulsion Laboratory, 30Cambridge, Institute of Astronomy, UK, 31Penn State University, Department of Astronomy and Astrophysics, 32Jet Propulsion Laboratory, 33University of California, Berkeley, Department of Physics, 34ASI Science Data Center, Italy, 35California Institute of Technology, Cahill Center for Astronomy and Astrophysics, 36Cambridge, Institute of Astronomy, UK, 37Jet Propulsion Laboratory, 38Purdue University, Department of Physics and Astronomy, 39Texas Tech University, Physics Department, 40Nagoya University, Center for Experimental Studies, Kobayashi-Maskawa Institute for the Origin of Particles and the Universe, 41University of Maryland, Physics Department, 42RIKEN, 43Univ. of Michigan in Ann Arbor, Astronomy Dept, 44Harvard-Smithsonian Center for Astrophysics, 45Istituto di Astrofisica e Planetologia Spaziali, INAF, 46Department of Astronomy/Steward Observatory, 47Lawrence Livermore National Laboratory, 48Jet Propulsion Laboratory, 49Department of Astronomy/Steward Observatory, 50NASA Goddard Space Flight Center, 51Tohoku University, Astronomical Institute, 52NASA Goddard Space Flight Center

This paper describes the Polarization Spectroscopic Telescope Array (PolSTAR), a mission proposed to NASA's 2014 Small Explorer (SMEX) announcement of opportunity. PolSTAR measures the linear polarization of 3-50 keV (requirement; goal: 2.5-70 keV) X-rays probing the behavior of matter, radiation and the very fabric of spacetime under the extreme conditions close to the event horizons of black holes, as well as in and around magnetars and neutron stars. Read More

Affiliations: 1SSL/UCB, 2SSL/UCB and Space Research Institute, Russian Academy of Sciences, 3ESO and Harvard, 4Clemson, 5CEA Saclay, 6SSL/UCB, 7Georgia College, 8CEA Saclay and Institut Universitaire de France

Here, we report on observations of two hard X-ray sources that were originally discovered with the INTEGRAL satellite: IGR J04059+5416 and IGR J08297-4250. We use the Chandra X-ray Observatory to localize the sources and then archival near-IR images to identify the counterparts. Both sources have counterparts in the catalog of extended 2 Micron All-Sky Survey sources, and the counterpart to IGR J04059+5416 has been previously identified as a galaxy. Read More


Multi-wavelength analysis of the young massive cluster VVV CL077 is presented for the first time. Our Chandra survey of this region enabled the detection of three X-ray emitting stellar members of the cluster, as well as a possible diffuse X-ray component that extends a few arcseconds from the cluster core with an intrinsic flux of (9+/-3)x10^-14 erg cm^-2 s^-1 in the 0.5-10 keV band. Read More

We present a catalog of 1415 X-ray sources identified in the Norma arm region Chandra survey (NARCS), which covers a 2 deg x 0.8 deg region in the direction of the Norma spiral arm to a depth of $\approx$20 ks. Of these sources, 1130 are point-like sources detected with $\geq3\sigma$ confidence in at least one of three energy bands (0. Read More

Affiliations: 1SSL-UC Berkeley, 2SSL-UC Berkeley, 3SSL-UC Berkeley, 4JPL-Caltech, 5PUC Chile, 6SSL-UC Berkeley, 7SSL-UC Berkeley, 8DTU Space, 9SSL-UC Berkeley, 10Columbia University, 11Columbia University, 12Caltech, 13Harvard University, 14Columbia University, 15NASA-GSFC

Results are presented for an initial survey of the Norma Arm gathered with the focusing hard X-ray telescope NuSTAR. The survey covers 0.2 deg$^2$ of sky area in the 3-79 keV range with a minimum and maximum raw depth of 15 ks and 135 ks, respectively. Read More

We report on CTIO/NEWFIRM and CTIO/OSIRIS photometric and spectroscopic observations of 20 new X-ray (0.5-10 keV) emitters discovered in the Norma Arm Region Chandra Survey (NARCS). NEWFIRM photometry was obtained to pinpoint the near-infrared counterparts of NARCS sources, while OSIRIS spectroscopy was used to help identify 20 sources with possible high mass X-ray binary properties. Read More

Affiliations: 1SSL/UCB, 2Columbia, 3ESO and Harvard, 4Universidad Diego Portales, 5Pontifica Universidad Catolica de Chile and SSI, 6SSL/UCB, 7SSL/UCB, 8DTU Space, 9SSL/UCB and LLNL, 10SSL/UCB, 11Harvard-Smithsonian CfA, 12Columbia, 13Caltech, 14SSL/UCB, 15INAF-IAPS, 16JPL, 17NASA/GSFC

During hard X-ray observations of the Norma spiral arm region by the Nuclear Spectroscopic Telescope Array (NuSTAR) in 2013 February, a new transient source, NuSTAR J163433-4738.7, was detected at a significance level of 8-sigma in the 3-10 keV bandpass. The source is consistent with having a constant NuSTAR count rate over a period of 40 ks and is also detected simultaneously by Swift at lower significance. Read More

Affiliations: 1SSL - UC Berkeley, 2SSL - UC Berkeley, 3CRESST/UMBC - NASA/GSFC, 4CEA-Saclay, 5Sternwarte/ECAP - Univ. Erlangen, Bamberg, 6Univ. of Cambridge

Detecting gamma-rays from microquasars is a challenging but worthwhile endeavor for understanding particle acceleration, the jet mechanism, and for constraining leptonic/hadronic emission models. We present results from a likelihood analysis on timescales of 1 d and 10 d of ~4 years worth of gamma-ray observations (0.1-10 GeV) by Fermi-LAT of Cyg X-1, Cyg X-3, GRS 1915+105, and GX 339-4. Read More

We report on the optical spectroscopic follow up observations of the candidate counterparts to four INTEGRAL sources: IGR J04069+5042, IGR J06552-1146, IGR J21188+4901 and IGR J22014+6034. The candidate counterparts were determined with Chandra, and the optical observations were performed with 1.5-m RTT-150 telescope (T\"{U}B\. Read More

We report on an observation of SGR 1627-41 made with the Chandra X-ray Observatory on 2011 June 16. Approximately three years after its outburst activity in 2008, the source's flux has been declining, as it approaches its quiescent state. For an assumed power-law spectrum, we find that the absorbed 2--10 keV flux for the source is $1. Read More

Affiliations: 1SSL/UC Berkeley, 2SSL/UC Berkeley, 3AIM and Institut Universitaire de France, 4AIM, 5Harvard University and CfA, 6Columbia University, 7Sabanci University, 8Middle East Technical University

We report on Chandra observations of 18 hard X-ray (>20 keV) sources discovered with the INTEGRAL satellite near the Galactic plane. For 14 of the INTEGRAL sources, we have uncovered one or two potential Chandra counterparts per source. These provide soft X-ray (0. Read More

Results are presented for XMM-Newton observations of five hard X-ray sources discovered by INTEGRAL in the direction of the Scutum Arm. Each source received more than 20 ks of effective exposure time. We provide refined X-ray positions for all five targets enabling us to pinpoint the most likely counterpart in optical/infrared archives. Read More

Affiliations: 1SSL/UC Berkeley, 2SSL/UC Berkeley, 3AIM - Univ. Paris VII and CEA Saclay, 4AIM - Univ. Paris VII and CEA Saclay, 5Columbia University, 6UC Berkeley, 7Harvard University and CfA

We report on Chandra X-ray and Parkes radio observations of IGR J11014-6103, which is a possible pulsar wind nebula with a complex X-ray morphology and a likely radio counterpart. With the superb angular resolution of Chandra, we find evidence that a portion of the extended emission may be related to a bow shock due to the putative pulsar moving through the interstellar medium. The inferred direction of motion is consistent with IGR J11014-6103 having been born in the event that produced the supernova remnant (SNR) MSH 11-61A. Read More

The Chandra High Resolution Camera observed the fields of five hard X-ray sources in order to help us obtain X-ray coordinates with sub-arcsecond precision. These observations provide the most accurate X-ray positions known for IGR J16393-4643 and for IGR J17091-3624. The obscured X-ray pulsar IGR J16393-4643 lies at R. Read More

We have performed the first sensitive X-ray observation of the low-mass X-ray binary SAX J1750.8-2900 in quiescence with XMM-Newton. The spectrum was fit to both a classical black body model, and a non-magnetized, pure hydrogen neutron star atmosphere model. Read More

Affiliations: 1Space Sciences Laboratory, University of California, Berkeley, USA, 2Space Sciences Laboratory, University of California, Berkeley, USA, 3Laboratoire AIM, CEA/IRFU - Université Paris Diderot - CNRS/INSU, CEA DSM/IRFU/SAp, Centre de Saclay, France, 4Dept. of Astronomy, University of California, Berkeley, USA

We present the first direct measurement of the spatial cross-correlation function of high-mass X-ray binaries (HMXBs) and active OB star-forming complexes in the Milky Way. This result relied on a sample containing 79 hard X-ray selected HMXBs and 458 OB associations. Clustering between the two populations is detected with a significance above 7-sigmas for distances < 1 kpc. Read More

Since the launch of INTEGRAL in 2002, about 300 new sources have been discovered. Understanding the nature of these objects is of prime importance for many aspects of astrophysics, such as the evolution of stars, population of sources (Galactic and extra-Galactic), and ultimately the physics powering them. However, their nature cannot be established from the soft gamma-ray observations. Read More

In 2009, Cygnus X-3 (Cyg X-3) became the first microquasar to be detected in the GeV {\gamma}-ray regime, via the satellites Fermi and AGILE. The addition of this new band to the observational toolbox holds promise for building a more detailed understanding of the relativistic jets of this and other systems. We present a rich dataset of radio, hard and soft X-ray, and {\gamma}-ray observations of Cyg X-3 made during a flaring episode in 2010 May. Read More

We summarize the results of our long-running campaign to help understand the nature of high-mass X-ray binaries (HMXBs), emphasizing recent Suzaku observations of IGR J16207-5129 and IGR J17391-3021. Thanks to the expanding ranks of HMXBs in our Galaxy, we are able to perform more reliable statistical analyses on the three currently-known sub-classes of HMXB: those with supergiant companions (SGXBs); those with Be companions (BEXBs); and the enigmatic Supergiant Fast X-ray Transients (SFXTs). We discuss new diagnostic tools, akin to the "Corbet diagram," in which HMXBs tend to segregate based on their dominant accretion mechanism. Read More

Affiliations: 1SSL/UC Berkeley, 2Univ. of Alberta, 3Columbia University, 4Univ. of Iowa, 5AIM - Univ. Paris VII and CEA Saclay, 6AIM - Univ. Paris VII and CEA Saclay, 7SSL/UC Berkeley

The field containing the candidate High Mass X-ray Binary IGR J01363+6610 was observed by XMM-Newton on 2009 July 31 for 28 ks. A Be star was previously suggested as the possible counterpart of the INTEGRAL source, and although Chandra, during a 2007 observation, did not detect an X-ray source at the position of the Be star, we find a variable source (XMMU J013549.5+661243) with an average X-ray flux of 2e-13 ergs/cm2/s (0. Read More

Observations with the INTEGRAL satellite have quadrupled the population of supergiant High Mass X-ray Binaries (HMXBs), revealed a previously hidden population of obscured supergiant HMXBs, and allowed the discovery of huge and fast transient flares in supergiant HMXBs. Apart from these 3 observational facts, has INTEGRAL allowed us to better understand these supergiant HMXBs? Do we have now a better understanding of the 3 populations of HMXBs, and of their accretion process, separated in the so-called Corbet diagram? Do we better apprehend the accretion process in the supergiant HMXBs, and what makes the fast transient flares so special, in the context of the clumpy wind model, and of the formation of transient accretion disks? In summary, has the increased population of supergiant HMXBs allowed a better knowledge of these sources, compared to the ones that were already known before the launch of INTEGRAL? We will review all these observational facts, comparing to the current models, to objectively estimate what is the INTEGRAL legacy on High Mass X-ray Binaries. Read More

Affiliations: 1SSL-UC Berkeley, 2SSL-UC Berkeley, 3CEA-Saclay, 4CEA-Saclay, 5CRESST-NASA/GSFC, 6ISDC-University of Geneva

An analysis of IGR J16207-5129 is presented based on observations taken with Suzaku. The data set represents ~80 ks of effective exposure time in a broad energy range between 0.5 and 60 keV, including unprecedented spectral sensitivity above 15 keV. Read More

Abridged : The various IBIS/ISGRI catalogues contain a large population of hard X-ray sources whose nature is still unknown. Even if the $>20$ keV positional uncertainty provided by ISGRI is unprecedented, it is still too large to pinpoint the counterpart at other wavelengths, which is the only secure way of obtaining a source identification. We continue the work of trying to reveal the nature of these hard X-ray sources, starting with analysis of X-ray data collected via focusing X-ray telescopes, in order to obtain arcsec accurate X-ray positions. Read More

We collected the parameters (position, absorption, spin, orbital period, etc..), when known, of all Galactic sources detected by INTEGRAL during its four first years of activity. Read More