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J/ApJ/788/123         IRTF J-band spectrum of Mrk 231           (Leighly+, 2014)

Evidence for active galactic nucleus feedback in the broad absorption lines and reddening of Mrk 231. Leighly K.M., Terndrup D.M., Baron E., Lucy A.B., Dietrich M., Gallagher S.C. <Astrophys. J., 788, 123 (2014)> =2014ApJ...788..123L (SIMBAD/NED BibCode)
ADC_Keywords: Galaxies, Seyfert ; Active gal. nuclei ; Spectra, infrared Keywords: quasars: absorption lines - quasars: individual: Mrk 231 Abstract: We present the first J-band spectrum of Mrk 231, which reveals a large He I* λ10830 broad absorption line with a profile similar to that of the well-known Na I broad absorption line. Combining this spectrum with optical and UV spectra from the literature, we show that the unusual reddening noted by Veilleux et al. (2013ApJ...764...15V) is explained by a reddening curve like those previously used to explain low values of total-to-selective extinction in Type Ia supernovae. The nuclear starburst may be the origin and location of the dust. Spatially resolved emission in the broad absorption line trough suggests nearly full coverage of the continuum emission region. The broad absorption lines reveal higher velocities in the He I* lines (produced in the quasar-photoionized H II region) compared with the Na I and Ca II lines (produced in the corresponding partially ionized zone). Cloudy simulations show that a density increase is required between the H II and partially ionized zones to produce ionic column densities consistent with the optical and IR absorption line measurements and limits, and that the absorber lies ∼100 pc from the central engine. These results suggest that the He I* lines are produced in an ordinary quasar BAL wind that impacts upon, compresses, and accelerates the nuclear starburst's dusty effluent (feedback in action), and the Ca II and Na I lines are produced in this dusty accelerated gas. This unusual circumstance explains the rarity of Na I absorption lines; without the compression along our line of sight, Mrk 231 would appear as an ordinary iron low-ionization, broad absorption line quasar. Description: Mrk 231 was observed using SpeX (Rayner et al. 2003PASP..115..362R) on the NASA Infrared Telescope Facility (IRTF) on 2010 April 24 for 30 minutes. A standard ABBA integration scheme was used. The A0 star HD 112623 was used for flux and telluric corrections. The spectra were reduced, and the telluric correction applied, in the standard manner using Spextool and accompanying software (Cushing et al. 2004PASP..116..362C; Vacca et al. 2003PASP..115..389V). The resolution measured from the arc lamp lines was about 12 Å FWHM, or 330 km/s in the vicinity of the absorption line. The galactic reddening in the direction of Mrk 231 is E(B-V)=0.0095, and we corrected for that using the CCM reddening curve (Cardelli et al. 1988ApJ...329L..33C). Objects: ---------------------------------------------------------------- RA (ICRS) DE Designation(s) ---------------------------------------------------------------- 12 56 14.23 +56 52 25.2 Mrk 231 = 2MASX J12561432+5652244 ---------------------------------------------------------------- File Summary:
FileName Lrecl Records Explanations
ReadMe 80 . This file table1.dat 26 4178 IRTF Spectrum
See also: J/ApJ/709/1257 : Spitzer-IRS spectra of Seyfert galaxies. II. (Tommasin+, 2010) J/AJ/143/83 : Properties of a sample of Seyfert 1 galaxies (Xu+, 2012) J/A+A/593/A30 : Detection of fast HI outflow in Mrk231 (Morganti+, 2016) Byte-by-byte Description of file: table1.dat
Bytes Format Units Label Explanations
1- 8 F8.6 um Wave Observed wavelength 10- 17 F8.3 10-19W/m2/nm Flux Flux density; 10-17 erg/s/cm2(1) 19- 26 F8.5 10-19W/m2/nm e_Flux Error in Flux (1)
Note (1): Corrected for Galactic Extinction.
History: From electronic version of the journal
(End) Prepared by [AAS], Tiphaine Pouvreau [CDS] 13-Jul-2017
The document above follows the rules of the Standard Description for Astronomical Catalogues.From this documentation it is possible to generate f77 program to load files into arrays or line by line

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