New Estimators of Black Hole Mass in Active Galactic Nuclei With Hydrogen Paschen Lines

Kim, Dohyeong; Im, Myungshin; Kim, Minjin

doi:10.1088/0004-637x/724/1/386

Cited by 65 publications

(132 citation statements)

References 40 publications

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“…comm. ) 7.3 Kim et al (2010) 7.3 M BH −σ * relation Gültekin et al (2009) 7.0 (+0.5 a ) Graham et al (2011) 6.7 b (+0.5 a ) Kormendy & Ho (2013) 7.4 (+0.5 a ) M BH −L bulge relation c Marconi & Hunt (2003) 8.0 Vika et al (2012) 8.2 8.4 Kormendy & Ho (2013) 8.4 M BH − M bulge relation Häring & Rix (2004) 6.0-6.8 Sani et al (2011) 6.6-7.1 Scott et al (2013) 5.1-6.6/6.9-7.5 d Kormendy & Ho (2013) 6.4-7.2…”

Section: The Central Black Holementioning

confidence: 99%

A low-luminosity type-1 QSO sample

Busch

Smajić

Scharwächter

et al. 2015

A&A

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Circumnuclear star formation and active galactic nucleus (AGN) feedback is believed to play a critical role in galaxy evolution. The low-luminosity quasi-stellar object (LLQSO) sample that contains 99 of the closest AGN with redshift z ≤ 0.06 fills the gap between the local AGN population and high-redshift QSOs that is essential to understand the AGN evolution with redshift. In this paper, we present the results of the near-infrared H-and K-integral field spectroscopy of the inner kiloparsecs of the LLQSO HE 1029-1831 with SINFONI. Line maps show that ionized hydrogen gas is located in spiral arms within the stellar bar and in a circumnuclear ring. Line fluxes and diagnostic line ratios indicate recent or ongoing star formation in the circumnuclear region and the presence of young and intermediate-age stellar populations in the bulge. In particular, we find traces of an intense starburst in the circumnuclear region that has begun around 100 Myr ago but has declined to a fraction of the maximum intensity now. We estimate the dynamical bulge mass and find that the galaxy follows published M BH −M bulge relations. However, bulge-disk decomposition of the K-band image with B reveals that HE 1029-1831 does not follow the M BH −L bulge relations of inactive galaxies. We conclude that the deviation from M BH −L bulge relations of inactive galaxies in this source is instead caused by young stellar populations and not by an undermassive black hole.

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Section: The Central Black Holementioning

confidence: 99%

A low-luminosity type-1 QSO sample

Busch

Smajić

Scharwächter

et al. 2015

A&A

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“…We assumed FWHM broad,Brγ FWHM broad,Hα and F broad,Brγ ≈ F broad,Hα /100 to scale the BL properties in the two bands. Note that, formally, the theoretical case-B is not applicable (but see Rhee & Larkin 2000;Zhou et al 2006;Kim et al 2010); nevertheless, we used it as a first approximation. According to Eq.…”

Section: Properties Of the Predicted Broad-line Regionmentioning

confidence: 99%

Is IRAS 01072+4954 a True-Seyfert 2?

Valencia-S.

Zuther

Eckart

et al. 2012

A&A

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In contrast to the predictions of the unified model, some X-ray unobscured Seyfert 2 galaxies have been discovered in the last decade. One of them, the starburst/Seyfert composite galaxy IRAS 01072+4954 (z = 0.0236), has a typical Type-1 X-ray emission, while its optical spectrum resembles an H ii galaxy and lacks the expected broad lines. We performed near-infrared integral-field observations of this object with the aim to determine the nature of its nuclear emission and to find indications for the existence or absence of a broad-line region. Several reasons have been proposed to explain this peculiar emission. We studied the validity of these hypotheses, including the possibility for this galaxy to be a True-Seyfert 2. We found little obscuration toward the nucleus A V = 2.5 mag, and a nuclear star-formation rate Σ SFR < 11.6 M yr −1 kpc −2 , which is below the average in Seyferts. Unresolved hot-dust emission with T ∼ 1150 K seems to indicate the presence of a torus with its axis close to the line of sight. We found that IRAS 01072+4954 hosts a low-mass black hole with an estimated mass of M BH ∼ 10 5 M . Its bolometric luminosity is L bol 2.5 × 10 42 erg s −1 , which yields a high accretion rate with an Eddington ratio λ Edd 0.2. If the relations found in more massive systems also apply to this case, then IRAS 01072+4954 should show broad emission lines with a FWHM broad ∼ (400−600) km s −1 . Indeed, some indications for such narrow broad-line components are seen in our data, but the evidence is not yet conclusive. This source therefore does not seem to be a True-Seyfert 2, but an extreme case of a narrow-line Seyfert 1, which, due to the faintness of the active nucleus, does not have strong Fe ii emission in the optical.

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“…We have estimated the black hole mass from the R−L relation (Kim et al 2010) for the broad Paα line and from the M − σ * relation (Merritt & Ferrarese 2001) with consistent results.…”

Section: Discussionmentioning

confidence: 55%

Unveiling the nucleus of NGC 7172

Smajić

Fischer

Zuther

et al. 2012

A&A

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Aims. We present the results of near-infrared (NIR) H + K European Southern Observatory SINFONI integral field spectroscopy (IFS) of the Seyfert 2 galaxy NGC 7172. We investigate the central 800 pc, concentrating on excitation conditions, morphology, and stellar content. NGC 7172 was selected from a sample of the ten nearest Seyfert 2 galaxies from the Veron-Cetty & Veron catalogue. All objects were chosen as test cases for adaptive optics (AO) assisted observations that allow a detailed study (at high spatial and spectral resolution) of the nuclear and host environments. NGC 7172 has a prominent dustlane crossing the central galaxy region from east to west, which makes it an ideal candidate to investigate the effect of obscuration by strong galactic extinction on (active) galaxies and their classification. Methods. The NIR is less influenced by dust extinction than optical light and is sensitive to the mass-dominating stellar populations. SINFONI integral field spectroscopy combines NIR imaging and spectroscopy and provides us with the opportunity to analyze several emission and absorption lines to investigate the stellar populations and ionization mechanisms over the 4 × 4 field of view (FOV). is predominantly inhabited by gas, dust, and an old K-M type giant stellar population. The gaseous, molecular, and stellar velocity maps show a related disturbed disk structure and similar velocities. Conclusions. We find evidence of nuclear activity located behind the prominent dustlane crossing the central region of the galaxy. The nucleus of NGC 7172, which is optically classified as a Seyfert 2 nucleus without any trace of broad emission lines, is a Seyfert 1 nucleus either surrounded by a molecular dust torus or hidden behind the strong galactic extinction. Our observation provides support for the unified model scheme. However, an evolutionary scenario cannot be ruled out by our observation.

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New Estimators of Black Hole Mass in Active Galactic Nuclei With Hydrogen Paschen Lines

Cited by 65 publications

References 40 publications

A low-luminosity type-1 QSO sample

A low-luminosity type-1 QSO sample

Is IRAS 01072+4954 a True-Seyfert 2?

Unveiling the nucleus of NGC 7172

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