Is IRAS 01072+4954 a True-Seyfert 2?

Valencia-S., M.; Zuther, J.; Eckart, A.; García-Marín, M.; Iserlohe, C.; Wright, Gillian

doi:10.1051/0004-6361/201219226

Cited by 22 publications

(28 citation statements)

References 152 publications

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“…15 = 120 pc. Thus, our values are in agreement with the expected star formation rate densities in Seyfert galaxies of (1−50) M yr −1 kpc −2 on hundreds of parsecs scales and (50−500) M yr −1 kpc −2 on tens of parsecs scales (Valencia-S. et al 2012a, and references therein). Furthermore, we can compare the star formation rate densities to the gas mass densities (estimated from the hot molecular gas mass) and find log(Σ gas,spot1 /M pc −2 ) = 3.7 and log(Σ gas,spot2 /M pc −2 ) = 3.6.…”

Section: Star Formation Ratessupporting

confidence: 90%

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: Star Formation Ratessupporting

confidence: 90%

A low-luminosity type-1 QSO sample

Busch

Smajić

Scharwächter

et al. 2015

A&A

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“…While low H 2 1−0S(1)/Brγ values appear to be characteristic of starbursts (H 2 1−0S(1)/Brγ < ∼ 0.6), classical Seyfert 1 and 2 galaxies also display a range of values (Rodríguez-Ardila et al 2004, 2005Riffel et al 2010) that are compatible with those measured in our sample. The [FeII]/Brγ ratio also shows values compatible with those observed in starbursts, although higher values would have been expected for Seyfert galaxies, such as NGC 5135 and NGC 7130 (Rodríguez-Ardila et al 2004;Riffel et al 2010;Valencia-S et al 2012). These galaxies show the highest values of the [FeII]/Brγ ratio of the whole sample, close to ∼2.0, and are similar to values reported for other Seyfert 2 galaxies (Blietz et al 1994).…”

Section: Characteristics Of the Near-ir Stacked Spectra Of Lirgs And supporting

confidence: 85%

“…This ratio is in principle not biased by extinction, and starburst galaxies and HII regions empirically exhibit lower H 2 /Brγ ratios, whereas Seyfert galaxies and LINERs show higher values (0.6 < ∼ H 2 1−0S(1)/Brγ < ∼ 2.0, Dale et al 2004;Rodríguez-Ardila et al 2005;Riffel et al 2010;Valencia-S et al 2012). …”

Section: Line Ratiosmentioning

confidence: 93%

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

López

Colina

Arribas

et al. 2012

A&A

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We present an atlas of a sample of local (z < 0.1) LIRGs (10) and ULIRGs (7) covering the luminosity range log(L IR /L ) = 11.1−12.4. The atlas is based on near-infrared H (1.45−1.85 μm) and K-band (1.95−2.45 μm) VLT-SINFONI integral field spectroscopy (IFS). The atlas presents the ionised, partially ionised, and warm molecular gas two-dimensional flux distributions and kinematics over an FoV of ∼3 × 3 kpc (LIRGs) and ∼12 × 12 kpc (ULIRGs) and with average linear resolutions of ∼0.2 kpc and ∼0.9 kpc, respectively. The different phases of the gas show a wide morphological variety with the nucleus as the brightest Brγ source for ∼33% of the LIRGs and ∼71% of the ULIRGs, whereas all the LIRGs and ULIRGs have their maximum H 2 emission in their nuclear regions. In LIRGs, the ionised gas distribution is dominated by the emission from the star-forming rings or giant HII regions in the spiral arms. The Brγ and [FeII] line at 1.644 μm trace the same structures, although the emission peaks at different locations in some of the objects, and the [FeII] seems to be more extended and diffuse. The ULIRG subsample is at larger distances and contains mainly pre-coalescence interacting systems. Although the peaks of the molecular gas emission and the continuum coincide in ∼71% of the ULIRGs, regions with intense Paα (Brγ) emission tracing luminous star-forming regions located at distances of 2−4 kpc away from the nucleus are also detected, usually associated with secondary nuclei or tidal tails. LIRGs have mean observed (i.e. uncorrected for internal extinction) SFR surface densities of about 0.4 to 0.9 M yr −1 kpc −2 over large areas (4−9 kpc 2 ) with peaks of about 2−2.5 M yr −1 kpc −2 in the smaller regions (0.16 kpc 2 ) associated with the nucleus of the galaxy or the brightest Brγ region. ULIRGs do have similar average SFR surface densities for the integrated emitting regions of ∼0.4 M yr −1 kpc −2 in somewhat larger areas (100−200 kpc 2 ) and for the Paα peak (∼2 M yr −1 kpc −2 in 4 kpc 2 ). The observed gas kinematics in LIRGs is primarily due to rotational motions around the centre of the galaxy, although local deviations associated with radial flows and/or regions of higher velocity dispersions are present. The ionised and molecular gas share the same kinematics (velocity field and velocity dispersion) to first order, showing slight differences in the velocity amplitudes (peak-to-peak) in some cases, whereas the average velocity dispersions are compatible within uncertainties. As expected, the kinematics of the ULIRG subsample is more complex, owing to the interacting nature of the objects of the sample.

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“…Zuther et al 2007;Smajić et al 2012;Valencia-S. et al 2012a;Smajić et al 2014;Busch et al 2015;Fazeli et al, in prep.). The NIR H + K-band contains several diagnostic lines: Hydrogen recombination lines (Paα and Brγ) can be excited by the AGN (in the broad-and narrow-line region), but are also tracers of young star formation.…”

Section: Introductionmentioning

confidence: 98%

“…Reduced spectra of the galaxies are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/587/A138 formation in the central kiloparsec (e.g. Böker et al 2008;Riffel et al 2009b;Bedregal et al 2009;Valencia-S. et al 2012a;Falcón-Barroso et al 2014;Busch et al 2015;Smajić et al 2015). IFS has also allowed spatially resolving inflows and outflows in many galaxies (e.g.…”

Section: Introductionmentioning

confidence: 99%

A low-luminosity type-1 QSO sample

Busch

Fazeli

Eckart

et al. 2016

A&A

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We present near-infrared (NIR) H + K-band long-slit spectra of eleven galaxies that were obtained with SOFI at the NTT (ESO). The galaxies are chosen from the low-luminosity type-1 quasi-stellar object (LLQSO) sample, which comprises the 99 closest (z ≤ 0.06) QSOs from the Hamburg/ESO survey for bright UV-excess QSOs. These objects are ideal targets to study the gap between local Seyfert galaxies and high-redshift quasars because they show much stronger AGN activity than local objects, but are still close enough for a detailed structural analysis. We fit hydrogen recombination, molecular hydrogen, and [Fe ii] lines after carefully subtracting the continuum emission. From the broad Paα components, we estimated black hole masses and enlarged the sample of LLQSOs that deviate from the M BH −L bulge relations of inactive galaxies from 12 to 16 objects. All objects show emission from hot dust (T ∼ 1200 K) as well as stellar contribution. However, the respective fractions vary strongly among the objects. More than half of the objects show H 2 emission lines, which indicate a large reservoir of molecular gas that is needed to feed the AGN and star formation. In the NIR diagnostic diagram all objects lie in the location of AGN-dominated objects. However, most of the objects show indications of star formation activity, suggesting that their offset location with respect to M BH -L bulge relations of inactive galaxies may be a consequence of overluminous bulges.

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Is IRAS 01072+4954 a True-Seyfert 2?

Cited by 22 publications

References 152 publications

A low-luminosity type-1 QSO sample

A low-luminosity type-1 QSO sample

VLT-SINFONI integral field spectroscopy of low-zluminous and ultraluminous infrared galaxies

A low-luminosity type-1 QSO sample

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