# Publications

## WISDOM project – VII. Molecular gas measurement of the supermassive black hole mass in the elliptical galaxy NGC 7052

Monthly Notices of the Royal Astronomical Society Oxford University Press 503 (2021) stab791

MD Smith, M Bureau, TA Davis, M Cappellari, L Liu, K Onishi, S Iguchi, EV North, M Sarzi, TG Williams

Supermassive black hole (SMBH) masses can be measured by resolving the dynamical influences of the SMBHs on tracers of the central potentials. Modern long-baseline interferometers have enabled the use of molecular gas as such a tracer. We present here Atacama Large Millimeter/submillimeter Array observations of the elliptical galaxy NGC 7052 at 0′′.11 (⁠37pc) resolution in the 12CO(2-1) line and 1.3 mm continuum emission. This resolution is sufficient to resolve the region in which the potential is dominated by the SMBH. We forward model these observations, using a multi-Gaussian expansion of a Hubble Space Telescope F814W image and a spatially constant mass-to-light ratio to model the stellar mass distribution. We infer an SMBH mass of 2.5±0.3×109M⊙ and a stellar I-band mass-to-light ratio of 4.6±0.2M⊙/L⊙,I (3σ confidence intervals). This SMBH mass is significantly larger than that derived using ionized gas kinematics, which however appears significantly more kinematically disturbed than the molecular gas. We also show that a central molecular gas deficit is likely to be the result of tidal disruption of molecular gas clouds due to the strong gradient in the central gravitational potential.

## WISDOM project – VIII. Multiscale feedback cycles in the brightest cluster galaxy NGC 0708

Monthly Notices of the Royal Astronomical Society Oxford University Press 503 (2021) 5179-5192

EV North, TA Davis, M Bureau, M Cappellari, M Gaspari, S Iguchi, L Liu, K Onishi, M Sarzi, MD Smith, TG Williams

<p>We present high-resolution (synthesized beam size 0<span tabindex="0" data-mathml="&lt;math xmlns=&quot;http://www.w3.org/1998/Math/MathML&quot;&gt;&lt;mrow class=&quot;MJX-TeXAtom-ORD&quot;&gt;&lt;msubsup&gt;&lt;mi&gt;&lt;/mi&gt;&lt;mrow class=&quot;MJX-TeXAtom-ORD&quot;&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;/mrow&gt;&lt;mrow class=&quot;MJX-TeXAtom-ORD&quot;&gt;&lt;mi class=&quot;MJX-variant&quot; mathvariant=&quot;normal&quot;&gt;&amp;#x2032;&lt;/mi&gt;&lt;mi class=&quot;MJX-variant&quot; mathvariant=&quot;normal&quot;&gt;&amp;#x2032;&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/mrow&gt;&lt;/math&gt;">&prime;&prime;..&prime;&prime;</span>088&nbsp;&times;&nbsp;0<span tabindex="0" data-mathml="&lt;math xmlns=&quot;http://www.w3.org/1998/Math/MathML&quot;&gt;&lt;mrow class=&quot;MJX-TeXAtom-ORD&quot;&gt;&lt;msubsup&gt;&lt;mi&gt;&lt;/mi&gt;&lt;mrow class=&quot;MJX-TeXAtom-ORD&quot;&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;/mrow&gt;&lt;mrow class=&quot;MJX-TeXAtom-ORD&quot;&gt;&lt;mi class=&quot;MJX-variant&quot; mathvariant=&quot;normal&quot;&gt;&amp;#x2032;&lt;/mi&gt;&lt;mi class=&quot;MJX-variant&quot; mathvariant=&quot;normal&quot;&gt;&amp;#x2032;&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/mrow&gt;&lt;/math&gt;">&prime;&prime;..&prime;&prime;</span>083 or 25&nbsp;&times;&nbsp;23&thinsp;pc<sup>2</sup>) Atacama Large Millimetre/submillimetre Array&nbsp;<sup>12</sup>CO(2&ndash;1) line and 236&thinsp;GHz continuum observations, as well as 5&thinsp;GHz enhanced Multi-Element Radio Linked Interferometer Network (e-MERLIN) continuum observations, of NGC&thinsp;0708; the brightest galaxy in the low-mass galaxy cluster Abell&thinsp;262. The line observations reveal a turbulent, rotating disc of molecular gas in the core of the galaxy, and a high-velocity, blueshifted feature &asymp;0<span tabindex="0" data-mathml="&lt;math xmlns=&quot;http://www.w3.org/1998/Math/MathML&quot;&gt;&lt;mrow class=&quot;MJX-TeXAtom-ORD&quot;&gt;&lt;msubsup&gt;&lt;mi&gt;&lt;/mi&gt;&lt;mrow class=&quot;MJX-TeXAtom-ORD&quot;&gt;&lt;mo&gt;.&lt;/mo&gt;&lt;/mrow&gt;&lt;mrow class=&quot;MJX-TeXAtom-ORD&quot;&gt;&lt;mi class=&quot;MJX-variant&quot; mathvariant=&quot;normal&quot;&gt;&amp;#x2032;&lt;/mi&gt;&lt;mi class=&quot;MJX-variant&quot; mathvariant=&quot;normal&quot;&gt;&amp;#x2032;&lt;/mi&gt;&lt;/mrow&gt;&lt;/msubsup&gt;&lt;/mrow&gt;&lt;/math&gt;">&prime;&prime;..&prime;&prime;</span>4 (&asymp;113&thinsp;pc) from its centre. The submillimetre continuum emission peaks at the nucleus, but extends towards this anomalous CO emission feature. No corresponding elongation is found on the same spatial scales at 5&thinsp;GHz with e-MERLIN. We discuss potential causes for the anomalous blueshifted emission detected in this source, and conclude that it is most likely to be a low-mass in-falling filament of material condensing from the hot intracluster medium via chaotic cold accretion, but it is also possible that it is a jet-driven molecular outflow. We estimate the physical properties this structure has in these two scenarios, and show that either explanation is viable. We suggest future observations with integral field spectrographs will be able to determine the true cause of this anomalous emission, and provide further evidence for interaction between quenched cooling flows and mechanical feedback on both small and large scales in this source.</p>

## The Evolution of NGC 7465 as Revealed by Its Molecular Gas Properties

ASTROPHYSICAL JOURNAL 909 (2021) ARTN 98

LM Young, DS Meier, M Bureau, A Crocker, TA Davis, S Topal

## Mass-gap Mergers in Active Galactic Nuclei

ASTROPHYSICAL JOURNAL 908 (2021) ARTN 194

H Tagawa, B Kocsis, Z Haiman, I Bartos, K Omukai, J Samsing

## MIGHTEE-HI: The H I emission project of the MeerKAT MIGHTEE survey

Astronomy and Astrophysics EDP Sciences 646 (2021) A35

N Maddox, B Frank, A Ponomareva, M Jarvis, E Adams, R Davé, T Oosterloo, M Santos, S Blyth, M Glowacki, R Kraan-Korteweg, W Mulaudzi, B Namumba, I Prandoni, S Rajohnson, K Spekkens, N Adams, R Bowler, J Collier, I Heywood, S Sekhar, A Taylor

We present the H I emission project within the MIGHTEE survey, currently being carried out with the newly commissioned MeerKAT radio telescope. This is one of the first deep, blind, medium-wide interferometric surveys for neutral hydrogen (H I) ever undertaken, extending our knowledge of H I emission to z = 0.6. The science goals of this medium-deep, medium-wide survey are extensive, including the evolution of the neutral gas content of galaxies over the past 5 billion years. Simulations predict nearly 3000 galaxies over 0 <  z <  0.4 will be detected directly in H I, with statistical detections extending to z = 0.6. The survey allows us to explore H I as a function of galaxy environment, with massive groups and galaxy clusters within the survey volume. Additionally, the area is large enough to contain as many as 50 local galaxies with H I mass < 108 M⊙, which allows us to study the low-mass galaxy population. The 20 deg2 main survey area is centred on fields with exceptional multi-wavelength ancillary data, with photometry ranging from optical through far-infrared wavelengths, supplemented with multiple spectroscopic campaigns. We describe here the survey design and the key science goals. We also show first results from the Early Science observations, including kinematic modelling of individual sources, along with the redshift, H I, and stellar mass ranges of the sample to date.

## Bow-shocks, nova shells, disc winds and tilted discs: the Nova-Like V341 Ara Has It All

Monthly Notices of the Royal Astronomical Society Oxford University Press 501 (2021) 1951-1969

N Castro Segura, C Knigge, JA Acosta-Pulido, R Fender, A Ponomareva, D Williams

V341 Ara was recently recognized as one of the closest (d ≃ 150 pc) and brightest (V ≃ 10) nova-like cataclysmic variables. This unique system is surrounded by a bright emission nebula, likely to be the remnant of a recent nova eruption. Embedded within this nebula is a prominent bow shock, where the system’s accretion disc wind runs into its own nova shell. In order to establish its fundamental properties, we present the first comprehensive multiwavelength study of the system. Long-term photometry reveals quasi-periodic, super-orbital variations with a characteristic time-scale of 10–16 d and typical amplitude of ≃1 mag. High-cadence photometry from theTransiting Exoplanet Survey Satellite (TESS) reveals for the first time both the orbital period and a ‘negative superhump’ period. The latter is usually interpreted as the signature of a tilted accretion disc. We propose a recently developed disc instability model as a plausible explanation for the photometric behaviour. In our spectroscopic data, we clearly detect antiphased absorption and emission-line components. Their radial velocities suggest a high mass ratio, which in turn implies an unusually low white-dwarf mass. We also constrain the wind mass-loss rate of the system from the spatially resolved [O III] emission produced in the bow shock; this can be used to test and calibrate accretion disc wind models. We suggest a possible association between V341 Ara and a ‘guest star’ mentioned in Chinese historical records in AD 1240. If this marks the date of the system’s nova eruption, V341 Ara would be the oldest recovered nova of its class and an excellent laboratory for testing nova theory.

## Eccentric Black Hole Mergers in Active Galactic Nuclei

ASTROPHYSICAL JOURNAL LETTERS 907 (2021) ARTN L20

H Tagawa, B Kocsis, Z Haiman, I Bartos, K Omukai, J Samsing

## The Evolution of Gas-Phase Metallicity and Resolved Abundances in Star-forming Galaxies at z ≈ 0.6 – 1.8

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2020)

S Gillman, A Tiley, A Swinbank, U Dudzevičiūtė, R Sharples, I Smail, C Harrison, AJ Bunker, M Bureau, M Cirasuolo, GE Magdis, T Mendel, JP Stott

&lt;jats:title&gt;Abstract&lt;/jats:title&gt; &lt;jats:p&gt;We present an analysis of the chemical abundance properties of &#x2248;650 star-forming galaxies at z&#xA0;&#x2248;&#xA0;0.6&#xA0;&#x2013;&#xA0;1.8. Using integral-field observations from the K&#xA0;-&#xA0;band Multi-Object Spectrograph (KMOS), we quantify the [N&#x2009;ii]/H&#x3B1; emission-line ratio, a proxy for the gas-phase Oxygen abundance within the interstellar medium. We define the stellar mass&#xA0;&#x2013;&#xA0;metallicity relation at z&#xA0;&#x2248;&#xA0;0.6&#xA0;&#x2013;&#xA0;1.0 and z&#xA0;&#x2248;&#xA0;1.2&#xA0;&#x2013;&#xA0;1.8 and analyse the correlation between the scatter in the relation and fundamental galaxy properties (e.g. H&#x3B1; star-formation rate, H&#x3B1; specific star-formation rate, rotation dominance, stellar continuum half-light radius and Hubble-type morphology). We find that for a given stellar mass, more highly star-forming, larger and irregular galaxies have lower gas-phase metallicities, which may be attributable to their lower surface mass densities and the higher gas fractions of irregular systems. We measure the radial dependence of gas-phase metallicity in the galaxies, establishing a median, beam smearing-corrected, metallicity gradient of &#x394;Z/&#x394;R=&#xA0;0.002&#xA0;&#xB1;&#xA0;0.004 dex kpc&#x2212;1, indicating on average there is no significant dependence on radius. The metallicity gradient of a galaxy is independent of its rest-frame optical morphology, whilst correlating with its stellar mass and specific star-formation rate, in agreement with an inside-out model of galaxy evolution, as well as its rotation dominance. We quantify the evolution of metallicity gradients, comparing the distribution of &#x394;Z/&#x394;R in our sample with numerical simulations and observations at z&#xA0;&#x2248;&#xA0;0&#xA0;&#x2013;&#xA0;3. Galaxies in our sample exhibit flatter metallicity gradients than local star-forming galaxies, in agreement with numerical models in which stellar feedback plays a crucial role redistributing metals.&lt;/jats:p&gt;

## Resolving the disc-halo degeneracy II: NGC 6946

Monthly Notices of the Royal Astronomical Society Oxford University Press 500 (2020) 3579-3593

S Aniyan, A Ponomareva, K Freeman, M Arnaboldi, O Gerhard, L Coccato, K Kuijken, M Merrifield

The mass-to-light ratio (M/L) is a key parameter in decomposing galactic rotation curves into contributions from the baryonic components and the dark halo of a galaxy. One direct observational method to determine the disc M/L is by calculating the surface mass density of the disc from the stellar vertical velocity dispersion and the scale height of the disc. Usually, the scale height is obtained from near-IR studies of edge-on galaxies and pertains to the older, kinematically hotter stars in the disc, while the vertical velocity dispersion of stars is measured in the optical band and refers to stars of all ages (up to ∼ 10 Gyr) and velocity dispersions. This mismatch between the scale height and the velocity dispersion can lead to underestimates of the disc surface density and a misleading conclusion of the sub-maximality of galaxy discs. In this paper we present the study of the stellar velocity dispersion of the disc galaxy NGC 6946 using integrated star light and individual planetary nebulae as dynamical tracers. We demonstrate the presence of two kinematically distinct populations of tracers which contribute to the total stellar velocity dispersion. Thus, we are able to use the dispersion and the scale height of the same dynamical population to derive the surface mass density of the disc over a radial extent. We find the disc of NGC 6946 to be closer to maximal with the baryonic component contributing most of the radial gravitational field in the inner parts of the galaxy (⁠Vmax(bar)=0.76(±0.14)Vmax⁠).

## WISDOM project – VI. Exploring the relation between supermassive black hole mass and galaxy rotation with molecular gas

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) 500 (2020) 1933-1952

MD Smith, M Bureau, TA Davis, M Cappellari, L Liu, K Onishi, S Iguchi, EV North, M Sarzi

<jats:title>ABSTRACT</jats:title> <jats:p>Empirical correlations between the masses of supermassive black holes (SMBHs) and properties of their host galaxies are well established. Among these is the correlation with the flat rotation velocity of each galaxy measured either at a large radius in its rotation curve or via a spatially integrated emission-line width. We propose here the use of the deprojected integrated CO emission-line width as an alternative tracer of this rotation velocity, which has already been shown useful for the Tully–Fisher (luminosity–rotation velocity) relation. We investigate the correlation between CO line widths and SMBH masses for two samples of galaxies with dynamical SMBH mass measurements, with spatially resolved and unresolved CO observations, respectively. The tightest correlation is found using the resolved sample of 25 galaxies as $\log (M_\mathrm{BH}/\mathrm{M_\odot })=(7.5\pm 0.1)+(8.5\pm 0.9)[\log (W_\mathrm{50}/\sin i \, \mathrm{km\, s}^{-1})-2.7]$, where MBH is the central SMBH mass, W50 is the full width at half-maximum of a double-horned emission-line profile, and i is the inclination of the CO disc. This relation has a total scatter of $0.6\,$ dex, comparable to those of other SMBH mass correlations, and dominated by the intrinsic scatter of $0.5\,$ dex. A tight correlation is also found between the deprojected CO line widths and the stellar velocity dispersions averaged within one effective radius. We apply our correlation to the COLD GASS sample to estimate the local SMBH mass function.</jats:p>

## The AGN fuelling/feedback cycle in nearby radio galaxies – III. 3D relative orientations of radio jets and CO discs and their interaction

Monthly Notices of the Royal Astronomical Society Oxford University Press 499 (2020) 5719-5731

I Ruffa, RA Laing, I Prandoni, R Paladino, P Parma, TA Davis, M Bureau

This is the third paper of a series exploring the multifrequency properties of a sample of eleven nearby low-excitation radio galaxies (LERGs) in the southern sky. We are conducting an extensive study of different galaxy components (stars, dust, warm and cold gas, radio jets) with the aim of better understanding the AGN fuelling/feedback cycle in LERGs. Here, we present new, deep, sub-kpc resolution Karl G. Jansky Very Large Array (JVLA) data for five sample sources at 10 GHz. Coupling these data with previously acquired Atacama Large Millimetre/submillimetre Array (ALMA) CO(2–1) observations and measurements of comparable quality from the literature, we carry out for the first time a full 3D analysis of the relative orientations of jet and disc rotation axes in six FR I LERGs. This analysis shows (albeit with significant uncertainties) that the relative orientation angles span a wide range (≈30○–60○). There is no case where both axes are accurately aligned and there is a marginally significant tendency for jets to avoid the disc plane. Our study also provides further evidence for the presence of a jet-CO disc interaction (already inferred from other observational indicators) in at least one source, NGC 3100. In this case, the limited extent of the radio jets, along with distortions in both the molecular gas and the jet components, suggest that the jets are young, interacting with the surrounding matter and rapidly decelerating.

## Jeans modelling of the Milky Way’s nuclear stellar disc

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2020)

MC Sormani, J Magorrian, F Nogueras-Lara, N Neumayer, R Schönrich, RS Klessen, A Mastrobuono-Battisti

&lt;jats:title&gt;Abstract&lt;/jats:title&gt; &lt;jats:p&gt;The nuclear stellar disc (NSD) is a flattened stellar structure that dominates the gravitational potential of the Milky Way at Galactocentric radii 30 &#x2272; R &#x2272; 300&#x2009;pc. In this paper, we construct axisymmetric Jeans dynamical models of the NSD based on previous photometric studies and we fit them to line-of-sight kinematic data of APOGEE and SiO maser stars. We find that (i) the NSD mass is lower but consistent with the mass independently determined from photometry by Launhardt et&#xA0;al. (2002). Our fiducial model has a mass contained within spherical radius r = 100&#x2009;pc of $M(r&amp;amp;lt;100\, {\rm pc}) = 3.9 \pm 1 \times 10^8 \, \rm M_\odot$ and a total mass of $M_{\rm NSD} = 6.9 \pm 2 \times 10^8 \, \rm M_\odot$. (ii) The NSD might be the first example of a vertically biased disc, i.e. with ratio between the vertical and radial velocity dispersion &#x3C3;z/&#x3C3;R &amp;amp;gt; 1. Observations and theoretical models of the star-forming molecular gas in the central molecular zone suggest that large vertical oscillations may be already imprinted at stellar birth. However, the finding &#x3C3;z/&#x3C3;R &amp;amp;gt; 1 depends on a drop in the velocity dispersion in the innermost few tens of parsecs, on our assumption that the NSD is axisymmetric, and that the available (extinction corrected) stellar samples broadly trace the underlying light and mass distributions, all of which need to be established by future observations and/or modelling. (iii) We provide the most accurate rotation curve to date for the innermost 500&#x2009;pc of our Galaxy.&lt;/jats:p&gt;

## SDSS-IV MaNGA: the indispensable role of bars in enhancing the central star formation of low-z galaxies

Monthly Notices of the Royal Astronomical Society Oxford University Press (OUP) (2020)

L Lin, C Li, C Du, E Wang, T Xiao, M Bureau, A Fraser-McKelvie, K Masters, L Lin, D Wake, L Hao

&lt;jats:title&gt;Abstract&lt;/jats:title&gt; &lt;jats:p&gt;We analyse two-dimensional maps and radial profiles of EW(H&#x3B1;), EW(H&#x3B4;A), and Dn(4000) of low-redshift galaxies using integral field spectroscopy from the MaNGA survey. Out of &#x2248;1400 nearly face-on late-type galaxies with a redshift z &amp;amp;lt; 0.05, we identify 121 &#x201C;turnover&#x201D; galaxies that each have a central upturn in EW(H&#x3B1;), EW(H&#x3B4;A) and/or a central drop in Dn(4000), indicative of ongoing/recent star formation. The turnover features are found mostly in galaxies with a stellar mass above &#x223C;1010 M&#x2299; and NUV-r colour less than &#x2248;5. The majority of the turnover galaxies are barred, with a bar fraction of 89&#xB1;3%. Furthermore, for barred galaxies the radius of the central turnover region is found to tightly correlate with one third of the bar length. Comparing the observed and the inward extrapolated star formation rate surface density, we estimate that the central SFR have been enhanced by an order of magnitude. Conversely, only half of the barred galaxies in our sample have a central turnover feature, implying that the presence of a bar is not sufficient to lead to a central SF enhancement. We further examined the SF enhancement in paired galaxies, as well as the local environment, finding no relation. This implies that environment is not a driving factor for central SF enhancement in our sample. Our results reinforce both previous findings and theoretical expectation that galactic bars play a crucial role in the secular evolution of galaxies by driving gas inflow and enhancing the star formation and bulge growth in the center.&lt;/jats:p&gt;

## Detecting Kozai–Lidov Imprints on the Gravitational Waves of Intermediate-mass Black Holes in Galactic Nuclei

The Astrophysical Journal American Astronomical Society 901 (2020) 125-125

B Deme, B-M Hoang, S Naoz, B Kocsis

## Binary Intermediate-mass Black Hole Mergers in Globular Clusters

The Astrophysical Journal American Astronomical Society 899 (2020) 149-149

A Rasskazov, G Fragione, B Kocsis

## Revealing the Intermediate Mass Black Hole at the Heart of Dwarf Galaxy NGC404 with Sub-parsec Resolution ALMA Observations

Monthly Notices of the Royal Astronomical Society Oxford University Press 496 (2020) 4061-4078

M Bureau, M Cappellari, L Liu, M Smith

We estimate the mass of the intermediate-mass black hole at the heart of the dwarf elliptical galaxy NGC 404 using Atacama Large Millimeter/submillimeter Array (ALMA) observations of the molecular interstellar medium at an unprecedented linear resolution of ≈0.5 pc, in combination with existing stellar kinematic information. These ALMA observations reveal a central disc/torus of molecular gas clearly rotating around the black hole. This disc is surrounded by a morphologically and kinematically complex flocculent distribution of molecular clouds, that we resolve in detail. Continuum emission is detected from the central parts of NGC 404, likely arising from the Rayleigh–Jeans tail of emission from dust around the nucleus, and potentially from dusty massive star-forming clumps at discrete locations in the disc. Several dynamical measurements of the black hole mass in this system have been made in the past, but they do not agree. We show here that both the observed molecular gas and stellar kinematics independently require a ≈ 5 × 105 M black hole once we include the contribution of the molecular gas to the potential. Our best estimate comes from the high-resolution molecular gas kinematics, suggesting the black hole mass of this system is 5.5+4.1−3.8×105 M (at the 99% confidence level), in good agreement with our revised stellar kinematic measurement and broadly consistent with extrapolations from the black hole mass – velocity dispersion and black hole mass – bulge mass relations. This highlights the need to accurately determine the mass and distribution of each dynamically important component around intermediate-mass black holes when attempting to estimate their masses.

## Spin Evolution of Stellar-mass Black Hole Binaries in Active Galactic Nuclei

The Astrophysical Journal American Astronomical Society 899 (2020) 26-26

H Tagawa, Z Haiman, I Bartos, B Kocsis

## The Sixth Data Release of the Radial Velocity Experiment (Rave). II. Stellar Atmospheric Parameters, Chemical Abundances, and Distances

ASTRONOMICAL JOURNAL 160 (2020) ARTN 83

M Steinmetz, G Guiglion, PJ McMillan, G Matijevic, H Enke, G Kordopatis, T Zwitter, M Valentini, C Chiappini, L Casagrande, J Wojno, B Anguiano, O Bienayme, A Bijaoui, J Binney, D Burton, P Cass, P de Laverny, K Fiegert, K Freeman, JP Fulbright, BK Gibson, G Gilmore, EK Grebel, A Helmi, A Kunder, U Munari, JF Navarro, Q Parker, GR Ruchti, A Recio-Blanco, W Reid, GM Seabroke, A Siviero, A Siebert, M Stupar, F Watson, MEK Williams, RFG Wyse, F Anders, T Antoja, D Birko, J Bland-Hawthorn, D Bossini, RA Garcia, I Carrillo, WJ Chaplin, Y Elsworth, B Famaey, O Gerhard, P Jofre, A Just, S Mathur, A Miglio, I Minchev, G Monari, B Mosser, A Ritter, TS Rodrigues, R-D Scholz, S Sharma, K Sysoliatina, RAVE Collaboration

## The Sixth Data Release of the Radial Velocity Experiment (RAVE). I. Survey Description, Spectra, and Radial Velocities

ASTRONOMICAL JOURNAL 160 (2020) ARTN 82

M Steinmetz, G Matijevic, H Enke, T Zwitter, G Guiglion, PJ McMillan, G Kordopatis, M Valentini, C Chiappini, L Casagrande, J Wojno, B Anguiano, O Bienayme, A Bijaoui, J Binney, D Burton, P Cass, P de Laverny, K Fiegert, K Freeman, JP Fulbright, BK Gibson, G Gilmore, EK Grebel, A Helmi, A Kunder, U Munari, JF Navarro, Q Parker, GR Ruchti, A Recio-Blanco, W Reid, GM Seabroke, A Siviero, A Siebert, M Stupar, F Watson, MEK Williams, RFG Wyse, F Anders, T Antoja, D Birko, J Bland-Hawthorn, D Bossini, RA Garcia, I Carrillo, WJ Chaplin, Y Elsworth, B Famaey, O Gerhard, P Jofre, A Just, S Mathur, A Miglio, I Minchev, G Monari, B Mosser, A Ritter, TS Rodrigues, R-D Scholz, S Sharma, K Sysoliatina, RAVE Collaboration

## Formation and Evolution of Compact-object Binaries in AGN Disks

ASTROPHYSICAL JOURNAL American Astronomical Society 898 (2020) ARTN 25

H Tagawa, Z Haiman, B Kocsis