Kinematic scaling relations of CALIFA galaxies: A dynamical mass proxy for galaxies across the Hubble sequence

Aquino-Ortíz, E.; Valenzuela, O.; Sanchez, Sebastian Francisco Sanchez; Hernández-Toledo, H. M.; Ávila-Reese, V.; Ven, Glenn van de; Rodríguez-Puebla, Aldo; Zhu, Ling; Mancillas, B.; Cano-Díaz, M.; García-Benito, R.

doi:10.1093/mnras/sty1522

Cited by 51 publications

(42 citation statements)

References 87 publications

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“…The blue hexagons are the cases with 2 galaxies detected within 100 kpc from the QSO LOS. Alcorn et al 2018;Aquino-Ortíz et al 2018), which combines the galaxy dispersion velocity, σ 7 , and its rotational velocity Vmax. Then, we use the following relation from Alcorn et al (2018):…”

Section: Stellar Massmentioning

confidence: 99%

MusE GAs FLOw and Wind (MEGAFLOW) – III. Galactic wind properties using background quasars

Schroetter

Bouché

Zabl

et al. 2019

Monthly Notices of the Royal Astronomical Society

123

141

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We present results from our on-going MusE GAs FLOw and Wind (MEGAFLOW) survey, which consists of 22 quasar lines-of-sight, each observed with the integral field unit (IFU) MUSE and the UVES spectrograph at the ESO Very Large Telescopes (VLT). The goals of this survey are to study the properties of the circum-galactic medium around z ∼ 1 star-forming galaxies. The absorption-line selected survey consists of 79 strong Mg ii absorbers (with rest-frame equivalent width (REW) 0.3Å) and, currently, 86 associated galaxies within 100 projected kpc of the quasar with stellar masses (M ) from 10 9 to 10 11 M . We find that the cool halo gas traced by Mg ii is not isotropically distributed around these galaxies from the strong bi-modal distribution in the azimuthal angle of the apparent location of the quasar with respect to the galaxy major-axis. This supports a scenario in which outflows are bi-conical in nature and co-exist with a coplanar gaseous structure extending at least up to 60 to 80 kpc. Assuming that absorbers near the minor axis probe outflows, the current MEGAFLOW sample allowed us to select 26 galaxy-quasar pairs suitable for studying winds. From this sample, using a simple geometrical model, we find that the outflow velocity only exceeds the escape velocity when M 4 × 10 9 M , implying the cool material is likely to fall back except in the smallest halos. Finally, we find that the mass loading factor η, the ratio between the ejected mass rate and the star formation rate (SFR), appears to be roughly constant with respect to the galaxy mass.

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Section: Stellar Massmentioning

confidence: 99%

MusE GAs FLOw and Wind (MEGAFLOW) – III. Galactic wind properties using background quasars

Schroetter

Bouché

Zabl

et al. 2019

Monthly Notices of the Royal Astronomical Society

123

141

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“…A measurement of the ionized gas velocity dispersion is needed to correctly determine the circular velocity and dynamical mass (e.g. Iorio et al 2017;Aquino-Ortíz et al 2018;Leung et al 2018). The low spectral resolution of CALIFA (275 km s −1 FWHM at λ Hα ) makes determining the ionized gas velocity dispersion difficult, if not impossible, for this sample (see Levy et al 2018).…”

Section: Implications For Galaxy Dynamical Mass Measurementsmentioning

confidence: 99%

The EDGE-CALIFA Survey: Evidence for Pervasive Extraplanar Diffuse Ionized Gas in Nearby Edge-on Galaxies

Levy

Bolatto

Sánchez

et al. 2019

ApJ

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We investigate the prevalence, properties, and kinematics of extraplanar diffuse ionized gas (eDIG) in a sample of 25 edge-on galaxies selected from the CALIFA survey. We measure ionized gas scale heights from Hα and find that 90% have measurable scale heights with a median of 0.8 +0.7 −0.4 kpc. From the Hα kinematics, we find that 60% of galaxies show a decrease in the rotation velocity as a function of height above the midplane. This lag is characteristic of eDIG, and we measure a median lag of 21 km s −1 kpc −1 which is comparable to lags measured in the literature. We also investigate variations in the lag with radius. HI lags have been reported to systematically decrease with galactocentric radius. We find both increasing and decreasing ionized gas lags with radius, as well as a large number of galaxies consistent with no radial lag variation, and investigate these results in the context of internal and external origins for the lagging ionized gas. We confirm that the [SII]/Hα and [NII]/Hα line ratios increase with height above the midplane as is characteristic of eDIG. The ionization of the eDIG is dominated by star-forming complexes (leaky HII regions). We conclude that the lagging ionized gas is turbulent ejected gas likely resulting from star formation activity in the disk as opposed to gas in the stellar thick disk or bulge. This is further evidence for the eDIG being a product of stellar feedback and for the pervasiveness of this WIM-like phase in many local star-forming galaxies.

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“…The differences are also reflected in many properties, including the galaxy integrated colours, star formation rates, rotation velocity, and velocity dispersion (e.g. Tinsley 1980;Kauffmann et al 2003;Delgado-Serrano et al 2010;Zhong et al 2010;Whitaker et al 2012;Aquino-Ortíz et al 2018;Eales et al 2018) The two populations can be separated fundamentally by differences in the baryonic angular momentum. In a lambda cold dark matter (ΛCDM) Universe angular momentum originates from tidal torques between dark matter haloes in the early Universe (Hoyle 1956).…”

Section: Introductionmentioning

confidence: 99%

The dynamics and distribution of angular momentum in HiZELS star-forming galaxies atz = 0.8–3.3

Gillman

Swinbank

Tiley

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We present adaptive optics assisted integral field spectroscopy of 34 star-forming galaxies at z = 0.8-3.3 selected from the HiZELS narrow-band survey. We measure the kinematics of the ionised interstellar medium on ∼1 kpc scales, and show that the galaxies are turbulent, with a median ratio of rotational to dispersion support of V / σ = 0.82 ± 0.13. We combine the dynamics with high-resolution rest-frame optical imaging and extract emission line rotation curves. We show that high-redshift starforming galaxies follow a similar power-law trend in specific angular momentum with stellar mass as that of local late type galaxies. We exploit the high resolution of our data and examine the radial distribution of angular momentum within each galaxy by constructing total angular momentum profiles. Although the stellar mass of a typical star-forming galaxy is expected to grow by a factor ∼ 8 in the ∼5 Gyrs between z ∼ 3.3 and z ∼ 0.8, we show that the internal distribution of angular momentum becomes less centrally concentrated in this period i.e the angular momentum grows outwards. To interpret our observations, we exploit the EAGLE simulation and trace the angular momentum evolution of star-forming galaxies from z ∼ 3 to z ∼ 0, identifying a similar trend of decreasing angular momentum concentration. This change is attributed to a combination of gas accretion in the outer disk, and feedback that preferentially arises from the central regions of the galaxy. We discuss how the combination of the growing bulge and angular momentum stabilises the disk and gives rise to the Hubble sequence.

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Kinematic scaling relations of CALIFA galaxies: A dynamical mass proxy for galaxies across the Hubble sequence

Cited by 51 publications

References 87 publications

MusE GAs FLOw and Wind (MEGAFLOW) – III. Galactic wind properties using background quasars

MusE GAs FLOw and Wind (MEGAFLOW) – III. Galactic wind properties using background quasars

The EDGE-CALIFA Survey: Evidence for Pervasive Extraplanar Diffuse Ionized Gas in Nearby Edge-on Galaxies

The dynamics and distribution of angular momentum in HiZELS star-forming galaxies atz = 0.8–3.3

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