Measuring stellar kinematics in galaxies with the near-infrared (2-0) (12) CO absorption bandhead

Gaffney, Niall; Lester, D. F.; Doppmann, Gregg

doi:10.1086/133517

Cited by 18 publications

(26 citation statements)

References 26 publications

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“…This particular value was chosen to ensure the presence of the CO(2−0) band head in near-infrared (NIR) K-band spectra. This stellar absorption feature can be used to derive the stellar kinematics of the host galaxy or to analyze stellar populations (Gaffney et al 1995;Fischer et al 2006). These selection criteria result in a sample of 99 galaxies that we call the LLQSO sample throughout the text (for more information see Bertram et al 2007).…”

Section: Introductionmentioning

confidence: 99%

A low-luminosity type-1 QSO sample

Busch

Zuther

Valencia-S.

et al. 2014

A&A

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Recognizing the properties of the host galaxies of quasi-stellar objects (QSOs) is essential for understanding the suspected coevolution of central supermassive black holes (BHs) and their host galaxies. Low-luminosity type-1 QSOs (LLQSOs) are ideal targets because of their small cosmological distance, which allows for a detailed structural analysis. We selected a subsample of the Hamburg/ESO survey for bright UV-excess QSOs that contains only the 99 nearest QSOs with redshift z ≤ 0.06. From this LLQSO sample, we observed 20 galaxies and performed aperture photometry and bulge-disk-decomposition with BUDDA on near-infrared J-, H-, and K-band images to separate disk, bulge, bar, and nuclear component. From the photometric decomposition of these 20 objects and visual inspection of images of another 26, we find that ∼50% of the hosts are disk galaxies and most of them (86%) are barred. Stellar masses, calculated from parametric models based on inactive galaxy colors, range from 2 × 10 9 M to 2 × 10 11 M with an average mass of 7 × 10 10 M . Black hole masses measured from single-epoch spectroscopy range from 1 × 10 6 M to 5 × 10 8 M with a median mass of 3 × 10 7 M . In comparison with higher-luminosity QSO samples, LLQSOs tend to have lower stellar and BH masses. Moreover, in the effective radius vs. mean surface-brightness projection of the fundamental plane, they lie in the transition area between luminous QSOs and normal galaxies. This can be seen as additional evidence that they populate a region intermediate between the local Seyfert population and luminous QSOs at higher redshift. This region has not been well studied so far. Eleven LLQSOs, for which we have reliable morphological decompositions and BH mass estimations, lie below the published BH mass vs. bulge luminosity relations for inactive galaxies. This can partially be explained if one assumes that the bulges of active galaxies contain much younger stellar populations than the bulges of inactive galaxies. Another possibility would be that their BHs are undermassive. This might indicate that the growth of the host spheroid precedes that of the BH.

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Section: Introductionmentioning

confidence: 99%

A low-luminosity type-1 QSO sample

Busch

Zuther

Valencia-S.

et al. 2014

A&A

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“…Later studies have substituted the use of the Ca triplet line with the CO absorption line at 2.29 m (and sometimes at 1.63 m) to study whether mergers lie on or near the fundamental plane (see Gaffney et al [1995] for a discussion of the use of the 2.29 m CO absorption line for kinematic studies). The switch to the CO line was motivated by studies of luminous and ultraluminous infrared galaxies (LIRGs and ULIRGs, respectively).…”

Section: Introductionmentioning

confidence: 99%

A Survey of Merger Remnants. II. The Emerging Kinematic and Photometric Correlations

Rothberg¹,

Joseph²

2006

Astron J

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This paper is the second in a series exploring the properties of 51 optically selected, single-nuclei merger remnants. Spectroscopic data have been obtained for a subsample of 38 mergers and combined with previously obtained infrared photometry to test whether mergers exhibit the same correlations as elliptical galaxies among parameters such as stellar luminosity and distribution, central stellar velocity dispersion ( 0 ), and metallicity. Paramount to the study is to test whether mergers lie on the fundamental plane. Measurements of 0 have been made using the Ca triplet absorption line at 8500 8 for all 38 mergers in the subsample. Additional measurements of 0 were made for two of the mergers in the subsample using the CO absorption line at 2.29 m. The results indicate that mergers show a strong correlation among the parameters of the fundamental plane but fail to show a strong correlation between 0 and metallicity (Mg 2 ). In contrast to earlier studies, the 0 values of the mergers are consistent with objects that lie somewhere between intermediate-mass and luminous giant elliptical galaxies. However, the discrepancies with earlier studies appear to correlate with whether the Ca triplet or CO absorption lines are used to derive 0 , with the latter almost always producing smaller values. Finally, the photometric and kinematic data are used to demonstrate for the first time that the central phase-space densities of mergers are equivalent to those in elliptical galaxies. This resolves a long-standing criticism of the merger hypothesis.

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“…Valentijn 1990). As shown by Gaffney et al (1995), the 12 CO absorption features at 2.29 µm, if not widely used, are a very efficient tool for measuring stellar kinematics in dusty environments. The age of the stellar populations can also be approached through the equivalent widths of these absorption 12 CO features (Doyon et al 1994).…”

Section: Introductionmentioning

confidence: 99%

Dynamics of embedded bars and the connection with AGN

Emsellem

Greusard

Combes

et al. 2001

A&A

147

174

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Abstract. We present new stellar kinematical profiles of four galaxy hosts of active galactic nuclei, using the 12 CO bandhead around 2.3 µm with the ISAAC/VLT spectrograph. We find that the nuclear bars or discs, embedded in large-scale primary bars, have all a decoupled kinematics, in the sense that the maximum of the rotational velocity occurs in the nuclear region. In three cases (NGC 1097, NGC 1808 and NGC 5728), the velocity dispersion displays a significant drop at the nucleus, a rarely observed phenomenon. We also detect kinematical asymmetries (m = 1 mode) along the nuclear bar major-axis of NGC 1808 and NGC 5728, dynamical counterparts of corresponding asymmetries in the surface brightness. We have derived simple dynamical models in an attempt to fit the kinematics of each galaxy and reconstruct the full velocity field. For all four targets, the fits are good, and confirm the presence of the decoupled nuclear components. These models cannot however reproduce the observed central drop in the dispersion. We suggest that this drop is due to a transient cold nuclear disc, fuelled by gas inflow along the bar, that has recently formed new stars.

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Measuring stellar kinematics in galaxies with the near-infrared (2-0) (12) CO absorption bandhead

Cited by 18 publications

References 26 publications

A low-luminosity type-1 QSO sample

A low-luminosity type-1 QSO sample

A Survey of Merger Remnants. II. The Emerging Kinematic and Photometric Correlations

Dynamics of embedded bars and the connection with AGN

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