K. O. Mason

Satellite Applications Catapult (United Kingdom)

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J. A. Nousek

Pennsylvania State University

A. A. Breeveld

University College London

N. Gehrels

Goddard Space Flight Center

M. Still

Ames Research Center

S. T. Holland

University of North Carolina at Greensboro

A. J. Blustin

University of Cambridge

T. Poole

University College London

S. Hunsberger

National Institute of Allergy and Infectious Diseases

P. Schady

University of Bath

C. Gronwall

Pennsylvania State University

Cooperative Institutions

National Institute for Astrophysics

University College London

Goddard Space Flight Center

University of Leicester

Pennsylvania State University

Brera Astronomical Observatory

Max Planck Society

Centre National de la Recherche Scientifique

Max Planck Institute for Extraterrestrial Physics

University of California, Berkeley

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AN ULTRASOFT EINSTEIN X-RAY SURVEY

Elsevier eBooks (1991)

F. A. Córdova T. Rodriguez-Bell F. R. Harnden J. F. Kartje K. O. Mason

10.1016/b978-0-08-037302-7.50010-0

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Citations (2)

GRB050219b: no swift UVOT detection of afterglow emission.

GRB Coordinates Network (2005)

S. Hunsberger A. A. Breeveld P. Roming K. O. Mason P. Schady

Swift

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Citations (1)

Optical and X-ray observations of 3U 0614+09

The Astrophysical Journal (1974)

A. F. Davidsen Roger F. Malina H. A. Smith Hyron Spinrad B. Margon

view Abstract Citations (33) References (12) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Optical and X-Ray Observations of 3u 0614+09 Davidsen, A. ; Malina, R. ; Smith, H. ; Spinrad, H. ; Margon, B. ; Mason, K. ; Hawkins, F. ; Sanford, P. Abstract Based on positional agreement, ultraviolet excess, and spectroscopic peculiarity, the identification of the X-ray source 3U 0614+09 with a faint blue star, previously suggested by Murdin et al. (1974) as a candidate, is established. Four days of X-ray observations at 1-3 A failed to show evidence for significant variability or eclipses. The possibility that this object may be very similar to Sco X-1, but at a distance of 4-8 kpc, is discussed. Publication: The Astrophysical Journal Pub Date: October 1974 DOI: 10.1086/181623 Bibcode: 1974ApJ...193L..25D Keywords: Hot Stars; Stellar Spectrophotometry; Variable Stars; X Ray Sources; Emission Spectra; Photographic Plates; Ultraviolet Spectra; X Rays; Astrophysics full text sources ADS | data products SIMBAD (1)

Variable star

10.1086/181623

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Citations (21)

GRB 050318: SWIFT-UVOT refined analysis.

GRB Coordinates Network (2005)

M. de Pasquale P. Boyd S. T. Holland M. Still V. La Parola

Swift

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On-orbit calibration of the Swift Ultraviolet/Optical Telescope (UVOT)

Proceedings of SPIE, the International Society for Optical Engineering/Proceedings of SPIE (2005)

M. Ivanushkina A. A. Breeveld T. Poole Cynthia H. James A. J. Blustin

The Ultraviolet and Optical telescope (UVOT) is one of the three instruments on board of the SWIFT observatory. UVOT is on the cutting edge of our ability to observe and eventually help scientists to understand gamma-ray bursts. As any space-based telescope it requires both pre-flight and on-orbit calibrations. This paper is the first of a pair of papers presenting the initial on-board calibration of the UVOT. In particular, we'll discuss distortion, large and small scale sensitivity variations and the telescope point spread function.

Swift

Optical telescope

Ultraviolet

On board

Orbit (dynamics)

Spitzer Space Telescope

Orbital mechanics

X-ray telescope

10.1117/12.617580

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GRB 050326: early observations with Swift-UVOT.

GCN (2005)

S. T. Holland M. Still V. La Parola A. Morgan S. Hunsberger

Swift

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XMM-Newton first-light observations of the Hickson galaxy group 16

Astronomy and Astrophysics (2001)

Martin Turner J. N. Reeves T. J. Ponman M. Arnaud Marco Barbera

This paper presents the XMM-Newton first-light observations of the Hickson-16 compact group of galaxies. Groups are possibly the oldest large-scale structures in the Universe, pre-dating clusters of galaxies, and are highly evolved. This group of small galaxies, at a redshift of 0.0132 (or 80 Mpc) is exceptional in the having the highest concentration of starburst or AGN activity in the nearby Universe. So it is a veritable laboratory for the study of the relationship between galaxy interactions and nuclear activity. Previous optical emission line studies indicated a strong ionising continuum in the galaxies, but its origin, whether from starbursts, or AGN, was unclear. Combined imaging and spectroscopy with the EPIC X-ray CCDs unequivocally reveals a heavily obscured AGN and a separately identified thermal (starburst) plasma, in NGC 835, NGC 833, & NGC 839. NGC 838 shows only starburst thermal emission. Starbursts and AGN can evidently coexist in members of this highly evolved system of merged and merging galaxies, implying a high probability for the formation of AGN as well as starbursts in post-merger galaxies.

Peculiar galaxy

10.1051/0004-6361:20000070

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Citations (34)

GRB 050319: Swift-UVOT detection of the afterglow.

GRB Coordinates Network (2005)

P. Boyd S. T. Holland M. Still V. La Parola S. Hunsberger

Swift

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Discovery of a Possible Dwarf Nova with the XMM-Newton Optical Monitor

AAS/High Energy Astrophysics Division #5 (2000)

D. Pandel F. A. Córdova K. O. Mason T. P. Sasseen R. Shirey

Nova (rocket)

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The UV spectrum of the narrow-line Seyfert 1 galaxy, REJ1034+396

E. M. Puchnarewicz K. O. Mason Aneta Siemiginowska

We present UV spectroscopy of RE1034+396, taken with the Faint Object Spectrograph on the Hubble Space Telescope. With a spectral resolution of ~1-2A FWHM and a typical S/N of ~15 per diode, this is one of the first detailed UV spectra of an object in the narrow-line Seyfert 1 (NLS1) class. The spectrum probes the physics and kinematics of the high-ionization and coronal line gas, and the strength and form of the big blue bump component in the UV. We detect many emission lines, including Lyman alpha, CIV1549, HeII1640, CIII]1909 and MgII2798. We also identify a feature at 2647A (in the rest-frame) with highly-ionized iron [FeXI]2649; a line of the same species ([FeXI]7892) has also been seen in the optical spectrum. The velocity widths of the UV lines are relatively narrow (FWHM<2000 km/s) and similar to those of the optical lines, which suggests that all line emission in REJ1034+396, ie. including that of high- and low-ionization species and the forbidden lines, may be dominated by an intermediate-velocity (FWHM~1000 km/s), intermediate-density (log Ne~7.5 cm-3) region of gas. The slope of the UV continuum (alpha~0.9) is soft (ie. red) relative to quasars and the UV-to-soft X-ray flux ratio is unusually low implying that the big blue bump component is very weak in the UV. The present epoch UV to soft X-ray continuum is consistent with earlier data, demonstrating that this extreme big blue bump component is also very stable, unlike many other NLS1s which show extreme patterns of variability.

Rest frame

Line (geometry)

Doubly ionized oxygen

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Citations (1)