The KMOS<sup>3D</sup> Survey: Rotating Compact Star-forming Galaxies and the Decomposition of Integrated Line Widths*

Wisnioski, Emily; Mendel, J. Trevor; Schreiber, N. M. Förster; Genzel, R.; Wilman, David J.; Wuyts, Stijn; Belli, Sirio; Beifiori, A.; Bender, R.; Brammer, Gabriel; Chan, J.; Davies, Richard; Fabricius, Maximilian; Fossati, M.; Galametz, A.; Lang, P.; Lutz, D.; Nelson, Erica J.; Momcheva, I.; Rosario, D. J.; Saglia, R.; Tacconi, L. J.; Tadaki, Ken-ichi; Übler, Hannah; Dokkum, Pieter van

doi:10.3847/1538-4357/aab097

Cited by 45 publications

(53 citation statements)

References 145 publications

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“…Adopting the same excitation ratio between CO (3-2) and CO (1-0) and the same COto-H 2 conversion factor, the molecular gas fractions and depletion times are also consistent with those of the general population of star forming galaxies in the PHIBBS survey (Tacconi et al 2018) and the ASPECS program (Aravena et al 2019). The issue with this explanation is that even though the axis ratios of the galaxies are high at b/a ≈ 0.8, they are close to the median of the vD15 sample (see also Wisnioski et al 2018). It is therefore unlikely that galaxies with b/a ≈ 0.8 are nearly face-on, unless the compact massive region of the size-mass plane is bid towards face-on galaxies.…”

Section: Discussionmentioning

confidence: 97%

Anomalously Narrow Line Widths of Compact Massive Star-forming Galaxies at z ∼ 2.3: A Possible Inclination Bias in the Size–Mass Plane

Mowla

Nelson

Dokkum

et al. 2019

ApJL

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Compact, massive star forming galaxies at z ∼ 2.5 are thought to be building the central regions of giant elliptical galaxies today. However, a significant fraction of these objects were previously shown to have much smaller Hα line widths than expected. A possible interpretation is that Hα emission from their central regions, where the highest velocities are expected, is typically obscured by dust.Here we present ALMA observations of the CO(3-2) emission line of three compact, massive galaxies with Hα line widths of FWHM(Hα)∼125-260 km s −1 to test this hypothesis. Surprisingly, in all three galaxies, the CO line width is similar to the Hα line width: we find FWHM(CO)∼165 km s −1 for all three galaxies whereas FWHM(CO)∼450-700 km s −1 was expected from a simple virial estimator. These results show that the narrow Hα linewidths of many compact massive star-forming galaxies are not due to preferential obscuration of the highest velocity gas. An alternative explanation for the narrow line widths is that the galaxies are disks that are viewed nearly face-on. We suggest that there may be an inclination bias in the size-mass plane, such that the apparent rest-frame optical sizes of face-on galaxies are smaller than those of edge-on galaxies. Although not conclusive, this hypothesis is supported by an observed anti-correlation between size and axis ratio of massive galaxies.

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Section: Discussionmentioning

confidence: 97%

Anomalously Narrow Line Widths of Compact Massive Star-forming Galaxies at z ∼ 2.3: A Possible Inclination Bias in the Size–Mass Plane

Mowla

Nelson

Dokkum

et al. 2019

ApJL

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“…The median velocity beam smearing correction factor for the rotation-dominated galaxies identified in Section 7 is 1.36, with a range from 1.08 − 1.97. However, inferred intrinsic Hα sizes can be 1 − 4× greater than the H-band sizes used to derive the corrections Wisnioski et al 2018;Wilman et al 2019). In these cases the beam-smearing corrections may be overestimated when using the H-band size as has been done for this work.…”

Section: Kinematic Parametersmentioning

confidence: 97%

“…• shed new light on dense core formation and quenching, by unveiling star-forming disks, gas outflows, and signs of rejuvenation events in compact SFGs and massive sub-MS galaxies (Belli et al 2017;Wisnioski et al 2018).…”

Section: Introductionmentioning

confidence: 99%

The KMOS^3D Survey: Data Release and Final Survey Paper*

Wisnioski

Schreiber

Fossati

et al. 2019

ApJ

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We present the completed KMOS 3D survey − an integral field spectroscopic survey of 739, log(M /M ) > 9, galaxies at 0.6 < z < 2.7 using the K-band Multi Object Spectrograph (KMOS) at the Very Large Telescope (VLT). KMOS 3D provides a population-wide census of kinematics, star formation, outflows, and nebular gas conditions both on and off the star-forming galaxy main sequence through the spatially resolved and integrated properties of Hα, [NII], and [SII] emission lines. We detect Hα emission for 91% of galaxies on the main sequence of star-formation and 79% overall. The depth of the survey has allowed us to detect galaxies with star-formation rates below 1 M yr −1 , as well as to resolve 81% of detected galaxies with ≥ 3 resolution elements along the kinematic major axis. The detection fraction of Hα is a strong function of both color and offset from the main sequence, with the detected and non-detected samples exhibiting different SED shapes. Comparison of Hα and UV+IR star formation rates (SFRs) reveal that dust attenuation corrections may be underestimated by 0.5 dex at the highest masses (log(M /M ) > 10.5). We confirm our first year results of a high rotation dominated fraction (monotonic velocity gradient and v rot /σ 0 > √ 3.36) of 77% for the full KMOS 3D sample. The rotation-dominated fraction is a function of both stellar mass and redshift with the strongest evolution measured over the redshift range of the survey for galaxies with log(M /M ) < 10.5. With this paper we include a final data release of all 739observed objects § .

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“…GMASS 0953 (also known as K20-ID5, GS3-19791, 3D-HST GS30274, e.g. Daddi et al 2004;Popping et al 2017;Wisnioski et al 2018) is a massive SFG at z 2.226 located in the Chandra Deep Field South (CDFS; Giacconi et al 2002) (see Table 1 for the main properties of the galaxy). It presents an irregular morphology ( Figure 1), visible in both the HST /WFC3 (H -band, 1.5 µm) and HST /ACS (z -band, 0.85 µm) images, which appears bright and compact in the central region (R eff,H−band ∼ 2.5 kpc, corresponding to 0.3 ; van der Wel et al 2014), showing also an off-nuclear emission to the west, interpreted as an asymmetric stellar disc or a merger remnant (Wisnioski et al 2018;van Dokkum et al 2015).…”

Section: Gmass 0953: a Global Portraitmentioning

confidence: 99%

A multiwavelength study of a massive, active galaxy at z ∼ 2: coupling the kinematics of the ionized and molecular gas

Loiacono

Talia

Fraternali

et al. 2019

Monthly Notices of the Royal Astronomical Society

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We report a multi-wavelength study of the massive (M 10 11 M ), z ∼ 2 starforming galaxy GMASS 0953, which hosts an obscured AGN. We combined nearinfrared observations of the GNIRS, SINFONI and KMOS spectrographs to study the kinematics of the [O III] λ5007 and Hα emission lines. Our analysis shows that GMASS 0953 may host an ionized disc extending up to 13 kpc, which rotates at a velocity of V ion = 203 +17 −20 km s −1 at the outermost radius. Evidence of rotation on a smaller scale (R ∼ 1 kpc) arises from the CO(J=6-5) line. The central velocity V CO = 320 +92 −53 km s −1 traced by the molecular gas is higher than V ion , suggesting that the galaxy harbors a multi-phase disc with a rotation curve that peaks in the very central regions. The galaxy appears well located on the z = 0 baryonic Tully-Fisher relation. We also discuss the possibility that the [O III] λ5007 and Hα velocity gradients are due to a galactic-scale wind. Besides, we found evidence of an AGN-driven outflow traced by a broad blueshifted wing affecting the [O III] λ5007 line, which presents a velocity offset ∆v = −535 ± 152 km s −1 from the systemic velocity. Because of the short depletion timescale (τ dep ∼ 10 8 yr) due to gas ejection and gas consumption by star formation activity, GMASS 0953 may likely evolve into a passive galaxy. However, the role of the AGN in depleting the gas reservoir of the galaxy is quite unclear because of the uncertainties affecting the outflow rate.

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The KMOS^3D Survey: Rotating Compact Star-forming Galaxies and the Decomposition of Integrated Line Widths*

Cited by 45 publications

References 145 publications

Anomalously Narrow Line Widths of Compact Massive Star-forming Galaxies at z ∼ 2.3: A Possible Inclination Bias in the Size–Mass Plane

Anomalously Narrow Line Widths of Compact Massive Star-forming Galaxies at z ∼ 2.3: A Possible Inclination Bias in the Size–Mass Plane

The KMOS^3D Survey: Data Release and Final Survey Paper*

A multiwavelength study of a massive, active galaxy at z ∼ 2: coupling the kinematics of the ionized and molecular gas

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The KMOS3D Survey: Rotating Compact Star-forming Galaxies and the Decomposition of Integrated Line Widths*

Cited by 45 publications

References 145 publications

Anomalously Narrow Line Widths of Compact Massive Star-forming Galaxies at z ∼ 2.3: A Possible Inclination Bias in the Size–Mass Plane

Anomalously Narrow Line Widths of Compact Massive Star-forming Galaxies at z ∼ 2.3: A Possible Inclination Bias in the Size–Mass Plane

The KMOS3D Survey: Data Release and Final Survey Paper*

A multiwavelength study of a massive, active galaxy at z ∼ 2: coupling the kinematics of the ionized and molecular gas

Contact Info

Product

Resources

About

The KMOS^3D Survey: Rotating Compact Star-forming Galaxies and the Decomposition of Integrated Line Widths*

The KMOS^3D Survey: Data Release and Final Survey Paper*