A low-luminosity type-1 QSO sample

Busch, G.; Zuther, J.; Valencia-S., M.; Moser, Lydia; Fischer, Sebastian; Eckart, A.; Scharwächter, J.; Gadotti, Dimitri A.; Wisotzki, L.

doi:10.1051/0004-6361/201322486

Cited by 48 publications

(107 citation statements)

References 81 publications

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“…Fischer et al (2006) have observed nine galaxies from the sample with the near-infrared (NIR) spectrograph ISAAC (VLT) and find that the spectra show signs for both AGN activity and star formation. In our NIR study (Busch et al , 2014, we find that the LLQSOs do not follow published M BH −L bulge relations for inactive galaxies. A reason could be massive star formation in the circumnuclear regions.…”

Section: Introductioncontrasting

confidence: 63%

“…All pixels with count level below will be masked. Busch et al (2014) give more details on the fitting process and limits of 2D-decomposition. Figure 2 shows the results of the 2D-decomposition of HE 1029-1831: in the upper row, from left to right the original K-band image, the B model image, and a residual image.…”

Section: Bulge-disk Decompositionmentioning

confidence: 99%

“…Furthermore, Läsker et al (2014) claim that, provided there has been a thorough decomposition, the correlation between black hole mass and total host galaxy luminosity could be just as tight as the correlation between black hole mass and bulge luminosity. In our recent study (Busch et al 2014), we have probed the M BH −L bulge relation of low-luminosity type-1 quasi-stellar objects (LLQSOs). We performed a careful decomposition of K-band images with the B-code (de Souza et al 2004;Gadotti 2008) and find that the bulges do not follow the published M BH −L bulge relations for inactive galaxies of Marconi & Hunt (2003), Vika et al (2012), , and Kormendy & Ho (2013).…”

Section: Introductionmentioning

confidence: 99%

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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: Introductioncontrasting

confidence: 63%

Section: Bulge-disk Decompositionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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A low-luminosity type-1 QSO sample

Busch

Smajić

Scharwächter

et al. 2015

A&A

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“…(ii) the observed black hole mass function (Graham et al 2007;Shankar et al 2009;Vika et al 2009;Davis et al 2014;Mutlu-Pakdil et al 2016) and Magorrian relation (Thornton et al 2008;Jiang et al 2011;Mathur et al 2012;Jiang et al 2013;Reines et al 2013;Scott et al 2013;Busch et al 2014;Sanghvi et al 2014;Yuan et al 2014) at low redshift (z 0.5);…”

Section: Galaxy and Black Hole Propertiesmentioning

confidence: 99%

Dark-ages reionization and galaxy formation simulation – X. The small contribution of quasars to reionization

Qin

Mutch

Poole

et al. 2017

Monthly Notices of the Royal Astronomical Society

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Motivated by recent measurements of the number density of faint AGN at high redshift, we investigate the contribution of quasars to reionization by tracking the growth of central supermassive black holes in an update of the Meraxes semi-analytic model. The model is calibrated against the observed stellar mass function at z ∼ 0.6 − 7, the black hole mass function at z 0.5, the global ionizing emissivity at z ∼ 2 − 5 and the Thomson scattering optical depth. The model reproduces a Magorrian relation in agreement with observations at z < 0.5 and predicts a decreasing black hole mass towards higher redshifts at fixed total stellar mass. With the implementation of an opening angle of 80 deg for quasar radiation, corresponding to an observable fraction of ∼23.4 per cent due to obscuration by dust, the model is able to reproduce the observed quasar luminosity function at z ∼ 0.6 − 6. The stellar light from galaxies hosting faint AGN contributes a significant or dominant fraction of the UV flux. At high redshift, the model is consistent with the bright end quasar luminosity function and suggests that the recent faint z ∼ 4 AGN sample compiled by Giallongo et al. (2015) includes a significant fraction of stellar light. Direct application of this luminosity function to the calculation of AGN ionizing emissivity consequently overestimates the number of ionizing photons produced by quasars by a factor of 3 at z ∼ 6. We conclude that quasars are unlikely to make a significant contribution to reionization.

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“…Although the minimization algorithms are different in these packages, we assume they bring similar results of the decomposition since they have been tested and compared by different authors (e.g. Häussler et al 2007Häussler et al , 2013Kim et al 2014;Busch et al 2014). Also, each of these codes has its advantages which will be noticed further.…”

Section: The 2d Decompositionmentioning

confidence: 99%

Does the stellar disc flattening depend on the galaxy type?

Mosenkov

Sotnikova

Решетников

et al. 2015

Monthly Notices of the Royal Astronomical Society

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We analyze the dependence of the stellar disc flatness on the galaxy morphological type using 2D decomposition of galaxies from the reliable subsample of the Edge-on Galaxies in SDSS (EGIS) catalogue. Combining these data with the retrieved models of the edge-on galaxies from the Two Micron All Sky Survey (2MASS) and the Spitzer Survey of Stellar Structure in Galaxies (S 4 G) catalogue, we make the following conclusions:(1) The disc relative thickness z 0 /h in the near-and mid-infrared passbands correlates weakly with morphological type and does not correlate with the bulge-to-total luminosity ratio B/T in all studied bands.(2) Applying an 1D photometric profile analysis overestimates the disc thickness in galaxies with large bulges making an illusion of the relationship between the disc flattening and the ratio B/T .(3) In our sample the early-type disc galaxies (S0/a) have both flat and "puffed" discs. The early spirals and intermediate-type galaxies have a large scatter of the disc flatness, which can be caused by the presence of a bar: barred galaxies have thicker stellar discs, on average. On the other hand, the late-type spirals are mostly thin galaxies, whereas irregular galaxies have puffed stellar discs.

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A low-luminosity type-1 QSO sample

Cited by 48 publications

References 81 publications

A low-luminosity type-1 QSO sample

A low-luminosity type-1 QSO sample

Dark-ages reionization and galaxy formation simulation – X. The small contribution of quasars to reionization

Does the stellar disc flattening depend on the galaxy type?

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