The H I Tully-Fisher relation of early-type galaxies

Heijer, Milan den; Oosterloo, Tom; Serra, P.; Józsa, G. I. G.; Kerp, J.; Morganti, Raffaella; Cappellari, Michele; Davis, Timothy A.; Duc, Pierre Alain; Emsellem, Éric; Krajnović, Davor; McDermid, Richard M.; Naab, T.; Weijmans, Anne-Marie; Zeeuw, P. T. de

doi:10.1051/0004-6361/201526879

Cited by 56 publications

(30 citation statements)

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“…A perfectly polar H i configuration can be relatively stable within an oblate mass distribution (which NGC 3998 is likely to have, see Cappellari et al 2013). Using the available data on the inclination of the H i (den Heijer et al 2015) and of the optical body (Krajnović et al 2011;Cappellari et al 2013) we find that the position angle between the H i and the symmetry plane of the stellar distribution is 80 • , but given the uncertainties, a perfectly polar configuration cannot be entirely excluded. In Fig.…”

Section: Atomic Gas In Ngc 3998mentioning

confidence: 91%

“…The radius of the inner, misaligned gas disc is ∼1 kpc. The rotation velocity is ∼250 km s −1 (den Heijer et al 2015) and the orbital time at this radius is ∼1.5 × 10 6 yr. Therefore, we conclude that the period of time during which the gas disc has been changing orientation within the 1 kpc radius is of the order of a few times 10 6 yr. Hopkins & Quataert (2011) argue that stellar torques can also produce orbit crossings and shocks in the gas, which causes the gas to lose angular momentum and accrete onto a central black hole.…”

Section: An Accretion Event and The Evolution Of The Gas Diskmentioning

confidence: 93%

“…The optical spectrum of NGC 3998 shows broad Hα emission lines (Heckman 1980;Devereux 2011) although it is formally classified as a LINER 1.9 (Ho et al 1997). Imaging studies of the ionised gas in this galaxy have revealed a small Hα disk of about 100 pc (Pogge et al 2000) surrounded by a larger (∼5 kpc), warped structure (Ford et al 1986;Sánchez-Gallego et al 2012).…”

Section: Overview Of Ngc 3998mentioning

confidence: 99%

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A rare example of low surface-brightness radio lobes in a gas-rich early-type galaxy: the story of NGC 3998

Frank

Morganti

Oosterloo

et al. 2016

A&A

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We study the nearby lenticular galaxy NGC 3998. This galaxy is known to host a low-power radio AGN with a kpc-size one-sided jet and a large, nearly polar H i disc. It is therefore a good system to study to understand the relation between the availability of cold-gas and the triggering of AGNs in galaxies. Our new WSRT data reveal two faint, S-shaped radio lobes extending out to ∼10 kpc from the galaxy centre. Remarkably, we find that the inner H i disc warps back towards the stellar mid-plane in a way that mirrors the warping of the radio lobes. We suggest that the polar H i disc was accreted through a minor merger, and that the torques causing it to warp in the inner regions are also responsible for feeding the AGN. The "S" shape of the radio lobes would then be due to the radio jets adapting to the changing angular momentum of the accreted gas. The extended radio jets are likely poorly collimated, which would explain their quick fading and, therefore, their rarity in galaxies similar to NGC 3998. The fuelling of the central super-massive black hole is likely occurring via "discrete events", suggested by the observed variability of the radio core and the extremely high core dominance, which we attribute to the formation and ejection of a new jet resulting from a recent fuelling event.

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Section: Atomic Gas In Ngc 3998mentioning

confidence: 91%

Section: An Accretion Event and The Evolution Of The Gas Diskmentioning

confidence: 93%

Section: Overview Of Ngc 3998mentioning

confidence: 99%

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A rare example of low surface-brightness radio lobes in a gas-rich early-type galaxy: the story of NGC 3998

Frank

Morganti

Oosterloo

et al. 2016

A&A

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“…For the early-type galaxies of the sample, the rotational velocity was tentatively derived from the same stellar mass-rotational velocity relation derived for late-type galaxies (den Heijer et al 2015). Although early-type systems do not follow the same scaling relations as spirals, this assumption is justified because we wish to test whether these typical cluster objects have been formed through the transformation of star-forming systems after a gasstripping phenomenon.…”

Section: Parametrisation Of the Star Formation Historymentioning

confidence: 99%

Quenching of the star formation activity in cluster galaxies

Boselli

Roehlly

Fossati

et al. 2016

A&A

119

155

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We study the star formation quenching mechanism in cluster galaxies by fitting the spectral energy distribution (SED) of the Herschel Reference Survey, a complete volume-limited K-band-selected sample of nearby galaxies including objects in different density regions, from the core of the Virgo cluster to the general field. The SEDs of the target galaxies were fitted using the CIGALE SED modelling code. The truncated activity of cluster galaxies was parametrised using a specific star formation history with two free parameters, the quenching age QA and the quenching factor QF. These two parameters are crucial for the identification of the quenching mechanism, which acts on long timescales when starvation processes are at work, but is rapid and efficient when ram pressure occurs. To be sensitive to an abrupt and recent variation of the star formation activity, we combined twenty photometric bands in the UV to far-infrared in a new way with three age-sensitive Balmer line absorption indices extracted from available medium-resolution (R ∼ 1000) integrated spectroscopy and with Hα narrow-band imaging data. The use of a truncated star formation history significantly increases the quality of the fit in HI-deficient galaxies of the sample, that is to say, in those objects whose atomic gas content has been removed during the interaction with the hostile cluster environment. The typical quenching age of the perturbed late-type galaxies is QA < ∼ 300 Myr whenever the activity of star formation is reduced by 50% < QF ≤ 80% and QA < ∼ 500 Myr for QF > 80%, while that of the quiescent early-type objects is QA 1−3 Gyr. The fraction of late-type galaxies with a star formation activity reduced by QF > 80% and with an HI-deficiency parameter HI − de f > 0.4 drops by a factor of ∼5 from the inner half virial radius of the Virgo cluster (R/R vir < 0.5), where the hot diffuse X-ray emitting gas of the cluster is located, to the outer regions (R/R vir > 4). The efficient quenching of the star formation activity observed in Virgo suggests that the dominant stripping process is ram pressure. We discuss the implication of this result in the cosmological context of galaxy evolution.

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“…In fact, the only populations of star-forming and dispersion-dominated systems at high stellar masses in the local Universe are the relatively rare and interaction-induced (U)LIRGs systems (e.g., Arribas et al 2014) and merging galaxies (e.g., the HI Rogues Gallery; Hibbard et al 2001). However, an Hi-based TFR relation was recently investigated for passive early-type galaxies as part of the Atlas 3D survey (den Heijer et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Deep MUSE observations in the HDFS

Contini

Épinat

Bouché

et al. 2016

A&A

123

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Aims. Whereas the evolution of gas kinematics of massive galaxies is now relatively well established up to redshift z ∼ 3, little is known about the kinematics of lower mass (M ≤ 10 10 M ) galaxies. We use MUSE, a powerful wide-field, optical integral-field spectrograph (IFS) recently mounted on the VLT, to characterize this galaxy population at intermediate redshift.Methods. We made use of the deepest MUSE observations performed so far on the Hubble Deep Field South (HDFS). This data cube, resulting from 27 h of integration time, covers a one arcmin 2 field of view at an unprecedented depth (with a 1σ emission-line surface brightness limit of 1×10 −19 erg s −1 cm −2 arcsec −2 ) and a final spatial resolution of ≈0.7 . We identified a sample of 28 resolved emission-line galaxies, extending over an area that is at least twice the seeing disk, spread over a redshift interval of 0.2 < z < 1.4. More than half of the galaxies are at z ∼ 0.3−0.7, which is a redshift range poorly studied so far with IFS kinematics. We used the public HST images and multiband photometry over the HDFS to constrain the stellar mass and star formation rate (SFR) of the galaxies and to perform a morphological analysis using Galfit, providing estimates of the disk inclination, disk scale length, and position angle of the major axis. We derived the resolved ionized gas properties of these galaxies from the MUSE data and model the disk (both in 2D and in 3D with GalPaK 3D ) to retrieve their intrinsic gas kinematics, including the maximum rotation velocity and velocity dispersion. Results. We build a sample of resolved emission-line galaxies of much lower stellar mass and SFR (by ∼1−2 orders of magnitude) than previous IFS surveys. The gas kinematics of most of the spatially resolved MUSE-HDFS galaxies is consistent with disk-like rotation, but about 20% have velocity dispersions that are larger than the rotation velocities and 30% are part of a close pair and/or show clear signs of recent gravitational interactions. These fractions are similar to what has been found in previous IFS surveys of more massive galaxies, indicating that the dynamical state of the ionized gas and the level of gravitational interactions of star-forming galaxies is not a strong function of their stellar mass. In the high-mass regime, the MUSE-HDFS galaxies follow the Tully-Fisher relation defined from previous IFS surveys in a similar redshift range. This scaling relation also extends to lower masses/velocities but with a higher dispersion. We find that 90% of the MUSE-HDFS galaxies with stellar masses below 10 9.5 M have settled gas disks. The MUSE-HDFS galaxies follow the scaling relations defined in the local Universe between the specific angular momentum and stellar mass. However, we find that intermediate-redshift, star-forming galaxies fill a continuum transition from the spiral to elliptical local scaling relations, according to the dynamical state (i.e., rotation-or dispersion-dominated) of the gas. This indicates that some galaxies may lose their angu...

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The H I Tully-Fisher relation of early-type galaxies

Cited by 56 publications

References 44 publications

A rare example of low surface-brightness radio lobes in a gas-rich early-type galaxy: the story of NGC 3998

A rare example of low surface-brightness radio lobes in a gas-rich early-type galaxy: the story of NGC 3998

Quenching of the star formation activity in cluster galaxies

Deep MUSE observations in the HDFS

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