skip to main content
OSTI.GOV title logo U.S. Department of Energy
Office of Scientific and Technical Information

Title: THE STRUCTURE OF HE 1104-1805 FROM INFRARED TO X-RAY

Abstract

The gravitationally lensed quasar HE 1104-1805 has been observed at a variety of wavelengths ranging from the mid-infrared to X-ray for nearly 20 yr. We combine flux ratios from the literature, including recent Chandra data, with new observations from the SMARTS telescope and Hubble Space Telescope, and use them to investigate the spatial structure of the central regions using a Bayesian Monte Carlo analysis of the microlensing variability. The wide wavelength coverage allows us to constrain not only the accretion disk half-light radius r {sub 1/2}, but the power-law slope ξ of the size-wavelength relation r {sub 1/2}∝λ{sup ξ}. With a logarithmic prior on the source size, the (observed-frame) R-band half-light radius log (r {sub 1/2}/cm) is 16.0{sub {sup −}{sup 0}{sup .}{sup 4{sub +}{sub 0}{sub .}{sub 3}}}, and the slope ξ is 1.0{sub {sup −}{sup 0}{sup .}{sup 5}{sup 6{sub +}{sub 0}{sub .}{sub 3}{sub 0}}}. We put upper limits on the source size in soft (0.4–1.2 keV) and hard (1.2–8 keV) X-ray bands, finding 95% upper limits on log (r {sub 1/2}/cm) of 15.33 in both bands. A linear prior yields somewhat larger sizes, particularly in the X-ray bands. For comparison, the gravitational radius, using a black hole mass estimated using the Hβ line, ismore » log (r{sub g} /cm) = 13.94. We find that the accretion disk is probably close to face-on, with cos i = 1.0 being four times more likely than cos i = 0.5. We also find probability distributions for the mean mass of the stars in the foreground lensing galaxy, the direction of the transverse peculiar velocity of the lens, and the position angle of the projected accretion disk's major axis (if not face-on)« less

Authors:
;  [1]; ;  [2];  [3]
  1. Department of Astronomy, The Ohio State University, 140 West 18th Avenue, Columbus, OH 43210 (United States)
  2. Homer L. Dodge Department of Physics and Astronomy, University of Oklahoma, Norman, OK 73019 (United States)
  3. Department of Physics and Astronomy, College of Charleston, Charleston, SC 29424 (United States)
Publication Date:
OSTI Identifier:
22364647
Resource Type:
Journal Article
Journal Name:
Astrophysical Journal
Additional Journal Information:
Journal Volume: 798; Journal Issue: 2; Other Information: Country of input: International Atomic Energy Agency (IAEA); Journal ID: ISSN 0004-637X
Country of Publication:
United States
Language:
English
Subject:
79 ASTROPHYSICS, COSMOLOGY AND ASTRONOMY; ACCRETION DISKS; BLACK HOLES; COMPARATIVE EVALUATIONS; GALAXIES; GRAVITATIONAL LENSES; KEV RANGE; MASS; MONTE CARLO METHOD; PROBABILITY; QUASARS; SPACE; STARS; TELESCOPES; VISIBLE RADIATION; X RADIATION

Citation Formats

Blackburne, Jeffrey A., Kochanek, Christopher S., Chen, Bin, Dai, Xinyu, and Chartas, George. THE STRUCTURE OF HE 1104-1805 FROM INFRARED TO X-RAY. United States: N. p., 2015. Web. doi:10.1088/0004-637X/798/2/95.
Blackburne, Jeffrey A., Kochanek, Christopher S., Chen, Bin, Dai, Xinyu, & Chartas, George. THE STRUCTURE OF HE 1104-1805 FROM INFRARED TO X-RAY. United States. https://doi.org/10.1088/0004-637X/798/2/95
Blackburne, Jeffrey A., Kochanek, Christopher S., Chen, Bin, Dai, Xinyu, and Chartas, George. 2015. "THE STRUCTURE OF HE 1104-1805 FROM INFRARED TO X-RAY". United States. https://doi.org/10.1088/0004-637X/798/2/95.
@article{osti_22364647,
title = {THE STRUCTURE OF HE 1104-1805 FROM INFRARED TO X-RAY},
author = {Blackburne, Jeffrey A. and Kochanek, Christopher S. and Chen, Bin and Dai, Xinyu and Chartas, George},
abstractNote = {The gravitationally lensed quasar HE 1104-1805 has been observed at a variety of wavelengths ranging from the mid-infrared to X-ray for nearly 20 yr. We combine flux ratios from the literature, including recent Chandra data, with new observations from the SMARTS telescope and Hubble Space Telescope, and use them to investigate the spatial structure of the central regions using a Bayesian Monte Carlo analysis of the microlensing variability. The wide wavelength coverage allows us to constrain not only the accretion disk half-light radius r {sub 1/2}, but the power-law slope ξ of the size-wavelength relation r {sub 1/2}∝λ{sup ξ}. With a logarithmic prior on the source size, the (observed-frame) R-band half-light radius log (r {sub 1/2}/cm) is 16.0{sub {sup −}{sup 0}{sup .}{sup 4{sub +}{sub 0}{sub .}{sub 3}}}, and the slope ξ is 1.0{sub {sup −}{sup 0}{sup .}{sup 5}{sup 6{sub +}{sub 0}{sub .}{sub 3}{sub 0}}}. We put upper limits on the source size in soft (0.4–1.2 keV) and hard (1.2–8 keV) X-ray bands, finding 95% upper limits on log (r {sub 1/2}/cm) of 15.33 in both bands. A linear prior yields somewhat larger sizes, particularly in the X-ray bands. For comparison, the gravitational radius, using a black hole mass estimated using the Hβ line, is log (r{sub g} /cm) = 13.94. We find that the accretion disk is probably close to face-on, with cos i = 1.0 being four times more likely than cos i = 0.5. We also find probability distributions for the mean mass of the stars in the foreground lensing galaxy, the direction of the transverse peculiar velocity of the lens, and the position angle of the projected accretion disk's major axis (if not face-on)},
doi = {10.1088/0004-637X/798/2/95},
url = {https://www.osti.gov/biblio/22364647}, journal = {Astrophysical Journal},
issn = {0004-637X},
number = 2,
volume = 798,
place = {United States},
year = {Sat Jan 10 00:00:00 EST 2015},
month = {Sat Jan 10 00:00:00 EST 2015}
}