Spectra of Markarian galaxies. III

Arakelyan, M. A.; Dibai, E. A.; Есипов, В. Ф.; Markaryan, B. E.

doi:10.1007/bf01001067

Cited by 4 publications

(4 citation statements)

References 2 publications

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“…It is the most luminous galaxy in the local Universe ( z < 0.1), the nuclear spectrum shows extreme broad emission lines and strong BAL systems, and the morphology is associated with a merger, etc. (Arakelian et al 1971; Adams 1972; Adams & Weedman 1972; Rieke & Low 1972, 1975; Boksenberg et al 1977, and others). It is important to remark that Sanders et al (1987), Bryant & Scoville (1996) and Downes & Solomon (1998) found a very high concentration of CO molecular gas in the nuclear region of Mrk 231 (3 × 10 9 M ⊙ , within a diameter of 1.0 arcsec, ∼814 pc).…”

Section: Programme and Observationsmentioning

confidence: 97%

“…Mrk 231 also shows very interesting spectral characteristics, dominated in the optical by extremely strong Fe ii and broad Balmer emission lines at Z em = 0.042 (Arakelian et al 1971; Adams & Weedman 1972; Boksenberg et al 1977). In addition, it shows remarkable absorption‐line systems: a clear stellar absorption at Z abs = 0.042 plus at least three strong BAL systems.…”

Section: Programme and Observationsmentioning

confidence: 99%

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Infrared mergers and infrared quasi-stellar objects with galactic winds - III. Mrk 231: an exploding young quasi-stellar object with composite outflow/broad absorption lines (and multiple expanding superbubbles)

Lípari

Terlevich

Zheng³

et al. 2005

Monthly Notices of the Royal Astronomical Society

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We present a study of outflow (OF) and broad absorption line (BAL) systems in Mrk 231, and in similar infrared (IR) quasi‐stellar objects (QSOs). This study is based mainly on one‐dimensional and two‐dimensional spectroscopy (obtained at La Palma/William Herschel Telescope, Hubble Space Telescope, International Ultraviolet Explorer, European Southern Observatory/New Technology Telescope, Kitt Peak National Observatory, Apache Point Observatory and Complejo Astronomico El Leoncito observatories) plus Hubble Space Telescope images. For Mrk 231, we report evidence that the extreme nuclear OF process has at least three main components on different scales, which are probably associated with: (i) the radio jet, at parsec scale; (ii) the extreme starburst at parsec and kiloparsec scale. This OF has generated at least four concentric expanding superbubbles and the BAL systems. Specifically, inside and very close to the nucleus the two‐dimensional spectra show the presence of an OF emission bump in the blend Hα+[N ii], with a peak at the same velocity of the main BAL‐I system (VEjection BAL‐I∼−4700 km s−1). This bump was more clearly detected in the area located at 0.6–1.5 arcsec (490–1220 pc), to the south‐west of the nucleus core, showing a strong and broad peak. In addition, in the same direction [at position angle (PA) ∼−120°, i.e. close to the PA of the small‐scale radio jet] at 1.7–2.5 arcsec, we also detected multiple narrow emission‐line components, with ‘greatly’ enhanced [N ii]/Hα ratio (very similar to the spectra of jets bow shocks). These results suggest that the BAL‐I system is generated in OF clouds associated with the parsec‐scale jet. The Hubble Space Telescope images show four (or possibly five) nuclear superbubbles or shells with radii r∼ 2.9, 1.5, 1.0, 0.6 and 0.2 kpc. For these bubbles, the two‐dimensional Hα velocity field map and two‐dimensional spectra show the following. (i) At the border of the more extended bubble (S1), a clear expansion of the shell with blueshifted velocities (with circular shape and at a radius r∼ 5.0 arcsec). This bubble shows a rupture arc – to the south – suggesting that the bubble is in the blowout phase. The axis of this rupture or ejection (at PA ∼ 00°) is coincident with the axis of the intermediate and large‐scale structures detected at radio wavelengths. (ii) In addition, in the three more external bubbles (S1, S2, S3), the two‐dimensional William Herschel Telescope spectra show multiple emission‐line components with OF velocities, of 〈VOF Bubble〉 S1, S2 and S3 =[−(650 − 420) ± 30], [−500 ± 30] and [−230 ± 30] km s−1. (iii) In the whole circumnuclear region (1.8 < r < 5 arcsec), the [N ii]/Hα and [S ii]/Hα narrow emission‐line ratios show high values (>0.8), which are consistent with low‐ionization nuclear emission‐line region/OF processes associated with fast velocity shocks. Therefore, we suggest that these giant bubbles are associated with the large‐scale nuclear OF component, which is generated – at least in part – by the extreme nuclear starburst: giant...

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Section: Programme and Observationsmentioning

confidence: 97%

Section: Programme and Observationsmentioning

confidence: 99%

Infrared mergers and infrared quasi-stellar objects with galactic winds - III. Mrk 231: an exploding young quasi-stellar object with composite outflow/broad absorption lines (and multiple expanding superbubbles)

Lípari

Terlevich

Zheng³

et al. 2005

Monthly Notices of the Royal Astronomical Society

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“…It was proposed by Sanders et al (1988) that most ULIRGs are powered by dust-enshrouded QSOs in the late phases of a merger. A classic example of this is Mrk 231, where the detection of broad ($10,000 km s À1 ) hydrogen emission lines (Arakelian et al 1971;Adams & Weedman 1972) and radio jets (Lonsdale et al 2003) provides direct evidence for the central active galactic nucleus (AGN ). The final state of a ULIRG may be a large elliptical galaxy with a central massive quiescent black hole (Kormendy & Sanders 1992).…”

Section: Introductionmentioning

confidence: 99%

ASpitzer Space TelescopeInfrared Spectrograph Survey of Warm Molecular Hydrogen in Ultraluminous Infrared Galaxies

Higdon

Armus

Higdon

et al. 2006

ApJ

130

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We have conducted a survey of ultraluminous infrared galaxies (ULIRGs) with the Infrared Spectrograph on the Spitzer Space Telescope, obtaining spectra from 5.0 to 38.5 m for 77 sources with 0:02 < z < 0:93. Observations of the pure rotational H 2 lines S(3) 9.67 m, S(2) 12.28 m, and S(1) 17.04 m are used to derive the temperature and mass of the warm molecular gas. We detect H 2 in 77% of the sample, and all ULIRGs with F 60 m > 2 Jy. The average warm molecular gas mass is $2 ; 10 8 M . High extinction, inferred from the 9.7 m silicate absorption depth, is not observed along the line of sight to the molecular gas. The derived H 2 mass does not depend on F 25 m /F 60 m , which has been used to infer either starburst or AGN dominance. Similarly, the molecular mass does not scale with the 25 or 60 m luminosities. In general, the H 2 emission is consistent with an origin in photodissociation regions associated with star formation. We detect the S(0) 28.22 m emission line in a few ULIRGs. Including this line in the model fits tends to lower the temperature by $50Y100 K, resulting in a significant increase in the gas mass. The presence of a cooler component cannot be ruled out in the remainder of our sample, for which we do not detect the S(0) line. The measured S(7) 5.51 m line fluxes in six ULIRGs implies $3 ; 10 6 M of hot ($1400 K ) H 2 . The warm gas mass is typically less than 1% of the cold gas mass derived from 12 CO observations.

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“…Mrk 231 has several blueshifted Broad Absorption Line (BAL) systems evident in the ultraviolet data. Adams (1972), Boksenberg et al (1977), Arakelian et al (1971), Boroson et al (1991), Rudy et al (1985) and others discuss three distinguishable absorption systems in Mrk 231. The most prominent is defined by Nai, Caii and Hei lines originating in gas with an outflow velocity ∼ 4200 km s −1 relative to the line emission seen in the source.…”

Section: Introductionmentioning

confidence: 99%

X‐Ray Observations of Markarian 231

Turner¹

1999

ApJ

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This paper presents new X-ray observations of Mrk 231, an active galaxy of particular interest due to its large infrared luminosity and the presence of several blueshifted broad absorption line (BAL) systems, a phenomenon observed in a small fraction of QSOs.A ROSAT HRI image of Mrk 231 is presented, this shows an extended region of soft X-ray emission, covering several tens of kpc, consistent with the extent of the host galaxy. An ASCA observation of Mrk 231 is also presented. Hard X-rays are detected but the data show no significant variability in X-ray flux. The hard X-ray continuum is heavily attenuated and X-ray column estimates range from ∼ 2 × 10 22 − 10 23 cm −2 depending on whether the material is assumed to be neutral or ionized, and on the model assumed for the extended X-ray component. These ASCA data provide only the second hard X-ray spectrum of a BAL AGN presented to date. The broad-band spectral-energy-distribution of the source is discussed. While Mrk 231 is X-ray weak compared to Seyfert 1 galaxies, it has an optical-to-X-ray spectrum typical of a QSO.

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Spectra of Markarian galaxies. III

Cited by 4 publications

References 2 publications

Infrared mergers and infrared quasi-stellar objects with galactic winds - III. Mrk 231: an exploding young quasi-stellar object with composite outflow/broad absorption lines (and multiple expanding superbubbles)

Infrared mergers and infrared quasi-stellar objects with galactic winds - III. Mrk 231: an exploding young quasi-stellar object with composite outflow/broad absorption lines (and multiple expanding superbubbles)

ASpitzer Space TelescopeInfrared Spectrograph Survey of Warm Molecular Hydrogen in Ultraluminous Infrared Galaxies

X‐Ray Observations of Markarian 231

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