The ATLAS3D project – XVIII. CARMA CO imaging survey of early-type galaxies

Alatalo, Katherine; Davis, Timothy A.; Bureau, Martin; Young, Lisa M.; Blitz, Leo; Crocker, Alison F.; Bayet, E.; Bois, Maxime; Bournaud, F.; Cappellari, Michele; Davies, Roger L.; Zeeuw, P. T. de; Duc, Pierre Alain; Emsellem, Éric; Khochfar, Sadegh; Krajnović, Davor; Küntschner, H.; Lablanche, Pierre Yves; Morganti, Raffaella; McDermid, Richard M.; Naab, Thorsten; Oosterloo, Tom; Sarzi, Marc; Scott, Nicholas; Serra, P.; Weijmans, Anne-Marie

doi:10.1093/mnras/sts299

Cited by 153 publications

(260 citation statements)

References 81 publications

Supporting

Mentioning

246

Contrasting

Order By: Relevance

“…The first of these contaminants is optically obscuring dust, that is ubiquitously present in ETGs with molecular gas (Alatalo et al 2013). To minimise dust extinction, our MGE models were constructed from HST F814LP images (the longest wavelength available).…”

Section: Luminous Mass Models Agn and Dustmentioning

confidence: 99%

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

Davis

Bureau

Onishi

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

106

View full text Add to dashboard Cite

As part of the mm-Wave Interferometric Survey of Dark Object Masses (WISDOM) project, we present an estimate of the mass of the supermassive black hole (SMBH) in the nearby fast-rotating early-type galaxy NGC4697. This estimate is based on Atacama Large Millimeter/submillimeter Array (ALMA) cycle-3 observations of the 12 CO(2-1) emission line with a linear resolution of 29 pc (0. 53). We find that NGC4697 hosts a small relaxed central molecular gas disc with a mass of 1.6×10 7 M , co-spatial with the obscuring dust disc visible in optical Hubble Space Telescope (HST) imaging. We also resolve thermal 1 mm continuum emission from the dust in this disc. NGC4697 is found to have a very low molecular gas velocity dispersion, σ gas =1.65 +0.68 −0.65 km s −1 . This seems to be partially because the giant molecular cloud mass function is not fully sampled, but other mechanisms such as chemical differentiation in a hard radiation field or morphological quenching also seem to be required. We detect a Keplerian increase of the rotation of the molecular gas in the very centre of NGC4697, and use forward modelling of the ALMA data cube in a Bayesian framework with the KIN-EMATIC MOLECULAR SIMULATION (KINMS) code to estimate a SMBH mass of (1.3 +0.18 −0.17 ) ×10 8 M and an i-band mass-to-light ratio of 2.14 +0.04 −0.05 M /L (at the 99% confidence level). Our estimate of the SMBH mass is entirely consistent with previous measurements from stellar kinematics. This increases confidence in the growing number of SMBH mass estimates being obtained in the ALMA era.

show abstract

Section: Luminous Mass Models Agn and Dustmentioning

confidence: 99%

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

Davis

Bureau

Onishi

et al. 2017

Monthly Notices of the Royal Astronomical Society

Self Cite

106

View full text Add to dashboard Cite

show abstract

“…A diverse range of observations and simulations was performed, at its core optical integralfield spectroscopic observations with the SAURON instrument (Bacon et al 2001), yielding detailed information on the stellar kinematics Emsellem et al 2011;Krajnović et al 2013a,b) and populations (Cappellari et al 2012;Scott et al 2013;McDermid et al 2014McDermid et al , 2015. In addition to single-dish molecular gas surveys (Combes et al 2007;, both H i and CO interferometric observations were obtained (Young et al 2008;Crocker et al 2011;Serra et al 2012;Alatalo et al 2013). The morphology and kinematics of the molecular gas are characterised in Davis et al (2013), while its physical conditions are discussed in Crocker et al (2012) and Bayet et al (2013).…”

Section: Atlas 3d Surveymentioning

confidence: 99%

A star formation study of the ATLAS^3Dearly-type galaxies with the AKARI all-sky survey

Kokusho

Kaneda

Bureau

et al. 2017

A&A

View full text Add to dashboard Cite

Context. The star formation properties of early-type galaxies (ETGs) are currently the subject of considerable interest, particularly whether they differ from those of gas-rich spirals. Aims. We perform a systematic study of star formation in a large sample of local ETGs using polycyclic aromatic hydrocarbon (PAH) and dust emission, focusing on the galaxies' star formation rates (SFRs) and star formation efficiencies (SFEs). Methods. Our sample is composed of the 260 ETGs from the ATLAS 3D survey, from which we use the cold gas measurements (H i and CO). The SFRs are estimated from stellar, PAH and dust fits to spectral energy distributions created from new AKARI measurements and literature data from WISE and 2MASS. Results. The mid-infrared luminosities of non-CO-detected galaxies are well correlated with their stellar luminosities, showing that they trace (circum)stellar dust emission. CO-detected galaxies show an excess above these correlations, uncorrelated with their stellar luminosities, indicating that they likely contain PAHs and dust of interstellar origin. PAH and dust luminosities of CO-detected galaxies show tight correlations with their molecular gas masses, and the derived current SFRs are typically 0.01 -1 M ⊙ yr −1 . These SFRs systematically decrease with stellar age at fixed stellar mass, while they correlate nearly linearly with stellar mass at fixed age. The majority of local ETGs follow the same star-formation law as local star-forming galaxies, and their current SFEs do not depend on either stellar mass or age. Conclusions. Our results clearly indicate that molecular gas is fueling current star formation in local ETGs, that appear to acquire this gas via mechanisms regulated primarily by stellar mass. The current SFEs of local ETGs are similar to those of local star-forming galaxies, indicating that their low SFRs are likely due to smaller cold gas fractions rather than a suppression of star formation.

show abstract

“…This has been interpreted as being due to interactions with the group environments or a recent minor galaxy merger (Serra et al 2012). This percentage decreases when focusing on H 2 only (Alatalo et al 2013;Davis et al 2013). Lagos et al (2014b, hereafter Paper I) explored the origin of the H I and H 2 gas contents of ETGs using a semi-analytic model of galaxy formation and showed that the observed gas fractions in ETGs arise in the model due to inefficient replenishment of the gas in ETGs as a result of both ram-pressure stripping of the hot gas and heating by active galactic nuclei (AGN), which prevents gas cooling from the hot halo.…”

mentioning

confidence: 99%

The origin of the atomic and molecular gas contents of early-type galaxies – II. Misaligned gas accretion

Lagos

Padilla

Davis

et al. 2015

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

We study the origin of the wide distribution of angles between the angular momenta of the stellar and gas components, α G,S , in early-type galaxies (ETGs). We use the GALFORM model of galaxy formation, set in the Λ cold dark matter framework, and coupled it with a Monte-Carlo simulation to follow the angular momenta flips driven by matter accretion onto haloes and galaxies. We consider a gas disk to be misaligned with respect to the stellar body if α G,S > 30 degrees. By assuming that the only sources of misaligments in galaxies are galaxy mergers, we place a lower limit of 2 − 5 per cent on the fraction of ETGs with misaligned gas/stellar components. These low fractions are inconsistent with the observed value of ≈ 42 ± 6 per cent in ATLAS 3D . In the more general case, in which smooth gas accretion in addition to galaxy mergers can drive misalignments, our calculation predicts that ≈ 46 per cent of ETGs have α G,S > 30 degrees. In this calculation, we find correlations between α G,S and stellar mass, cold gas fraction and star formation rate, such that ETGs with high masses, low cold gas fractions and low star formation rates are more likely to display aligned cold gas and stellar components. We confirm these trends observationally for the first time using ATLAS 3D data. We argue that the high fraction of misaligned gas discs observed in ETGs is mostly due to smooth gas accretion (e.g. cooling from the hot halo of galaxies) which takes place after most of the stellar mass of the galaxy is in place and comes misaligned with respect to the stellar component. Galaxies that have accreted most of their cold gas content prior to the time where most of the stellar mass was in place show aligned components.

show abstract

The ATLAS3D project – XVIII. CARMA CO imaging survey of early-type galaxies

Cited by 153 publications

References 81 publications

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

A star formation study of the ATLAS^3Dearly-type galaxies with the AKARI all-sky survey

The origin of the atomic and molecular gas contents of early-type galaxies – II. Misaligned gas accretion

Contact Info

Product

Resources

About

The ATLAS3D project – XVIII. CARMA CO imaging survey of early-type galaxies

Cited by 153 publications

References 81 publications

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

WISDOM Project – II. Molecular gas measurement of the supermassive black hole mass in NGC 4697

A star formation study of the ATLAS3Dearly-type galaxies with the AKARI all-sky survey

The origin of the atomic and molecular gas contents of early-type galaxies – II. Misaligned gas accretion

Contact Info

Product

Resources

About

A star formation study of the ATLAS^3Dearly-type galaxies with the AKARI all-sky survey