Further infrared and millimeter observations of Markarian 231

Joyce, R. R.; Knacke, R. F.; Simón, M.; Young, ET

doi:10.1086/129827

Cited by 6 publications

(6 citation statements)

References 7 publications

(8 reference statements)

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“…The power-law index of model 1(d) has a 95% confidence range of a = 1.1 (+0.58,-0.44), where f v 00 v~a, consistent with the best-fit value of 1.26 found by Roche et al (1983). The observed average index between 3 and 20 jum of a ~ 1.5 (Joyce et al 1975;Rieke 1976) lies within our range. Boksenberg et al (1977) have presented two models for Mrk 231 which are consistent with their visual observations.…”

Section: A Markarian 231supporting

confidence: 82%

Dust in the nuclei of the Seyfert galaxies Markarian 231 and NGC 4151

Jones

Worrall

Rodríguez-Espinosa

et al. 1984

PASP

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We report 8-13 pm grating-spectrometer observations of Mrk231 and NGC 4151. The Mrk 231 data can be fitted to various thermal dust emission models or a single power law, with dust extinction. In all the model fits, except for that of graphite and silicon carbide grain emission, a component of silicate absorption of optical depth t 9 7 > 0.7 is required. Confirming published work, we rule out the absorption being at the redshift of the low-redshift absorption-line system. The high values of t 9 7 do not give ratios to the galaxy's visual extinction which are comparable to those of galactic H II regions. We report weak evidence for a 10-pm absorption feature in NGC 4151. This is somewhat contrary to expectation, since the visual extinction of NGC 4151 is lower than that of Mrk 231, and since there is evidence to support a nonthermal rather than thermal dust origin for the infrared continuum emission.

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Section: A Markarian 231supporting

confidence: 82%

Dust in the nuclei of the Seyfert galaxies Markarian 231 and NGC 4151

Jones

Worrall

Rodríguez-Espinosa

et al. 1984

PASP

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“…All observations used a long integration on a bright quasar to calibrate the passband, and alternated integrations between a gain calibrator (1419+543) and Mrk 231. We then used the Mrk 231 3mm continuum source (Joyce et al 1975) to self calibrate. The self calibration step was able to mitigate atmospheric fluctuations for the longer baseline arrays.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Escape, Accretion, or Star Formation? The Competing Depleters of Gas in the Quasar Markarian 231

Alatalo

2015

ApJ

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We report on high resolution CO(1-0), CS(2-1) and 3mm continuum Combined Array for Research in Millimeter Astronomy (CARMA) observations of the molecular outflow host and nearest quasar Markarian 231. We use the CS(2-1) measurements to derive a dense gas mass within Mrk 231 of 1.8 ± 0.3 × 10 10 M ⊙ , consistent with previous measurements. The CS(2-1) data also seem to indicate that the molecular disk of Mrk 231 is forming stars at about normal efficiency. The high resolution CARMA observations were able to resolve the CO(1-0) outflow into two distinct lobes, allowing for a size estimate to be made and further constraining the molecular outflow dynamical time, further constraining the molecular gas escape rate. We find that 15% of the molecular gas within the Mrk 231 outflow actually exceeds the escape velocity in the central kiloparsec. Assuming that molecular gas is not constantly being accelerated, we find the depletion timescale of molecular gas in Mrk 231 to be 49 Myr, rather than 32 Myr, more consistent with the poststarburst stellar population observed in the system.

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“…(1) NED, IRSA, Clemens et al (2008), (2) Klaas et al (2001), (3) Roche & Chandler (1993), (4) Joyce & Simon (1976), (5) Rieke (1978), (6) Rieke (1976), (7) Joyce et al (1975), (8) Weedman et al (2005), (9) Rigopoulou et al (1996), (10) Carico et al (1992), (11) Farrah et al (2003), (12) Dunne & Eales (2001), (13) Dunne et al (2000), (14) Maiolino & Rieke (1995), (15) Chini et al (1986), ( Hwang et al (1999), (33) Albrecht et al (2007), (34) Alonso-Herrero et al (2003).…”

Section: Samplementioning

confidence: 99%

Modelling the spectral energy distribution of ULIRGs

Vega

Clemens²,

Bressan

et al. 2008

A&A

101

131

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Aims. By using the spectral energy distribution (SED) from the near-infrared to the radio of a statistically significant number of luminous infrared galaxies we determine important physical parameters for this population of objects. In particular we constrain the optical depth towards the luminosity source, the star formation rate, the star formation efficiency and the AGN fraction. Methods. We fit the near-infrared to radio spectral energy distributions of a sample of 30 luminous and ultra-luminous infrared galaxies with pure starburst models or models that include both starburst and AGN components. Results. We find that although about half of our sample have best-fit models that include an AGN component, only 30% (9/30) have an AGN that accounts for more than 10% of the infrared luminosity from 8 to 1000 μm, whereas all have an energetically dominant starburst. Our derived AGN fractions are generally in good agreement with measurements of the mid-infrared line ratios, Ne[V]/Ne [II] and O[IV]/Ne[II] by Spitzer IRS, but much lower than those derived from PAH equivalent widths or the mid-infrared spectral slope. Our models determine the mass of dense molecular gas within which active star formation takes place via the extinction required to reproduce the infrared part of the SED. Assuming that this mass is that traced by the HCN molecule, we reproduce the observed linear relation between HCN flux and infrared luminosity found previously. We also find that the star formation efficiency, as defined by the current star formation rate per unit molecular gas mass, falls as the starburst ages. Conclusions. If the evolution of ULIRGs includes a phase in which an AGN contributes an important fraction to the infrared luminosity, this phase should last an order of magnitude less time than the starburst phase. However, we find no convincing evidence that an energetically important AGN is associated with a particular phase of the starburst. Because the mass of dense molecular gas that we derive is consistent with observations of the HCN molecule, it should be possible to estimate the mass of dense, star-forming molecular gas in such objects when molecular line data are not available.

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Further infrared and millimeter observations of Markarian 231

Abstract: New infrared and 3.3 millimeter observations of the Seyfert galaxy, Markarian 231, are reported. Thermal and nonthermal models of the radiation source are discussed although it is not possible to specify a unique model based on these data.

Cited by 6 publications

References 7 publications

Dust in the nuclei of the Seyfert galaxies Markarian 231 and NGC 4151

Dust in the nuclei of the Seyfert galaxies Markarian 231 and NGC 4151

Escape, Accretion, or Star Formation? The Competing Depleters of Gas in the Quasar Markarian 231

Modelling the spectral energy distribution of ULIRGs

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