The KMOS Redshift One Spectroscopic Survey (KROSS): dynamical properties, gas and dark matter fractions of typical<i>z</i>∼ 1 star-forming galaxies

Stott, John P.; Swinbank, A. M.; Johnson, H. L.; Tiley, Alfred L.; Magdis, G.; Bower, Richard G.; Bunker, Andrew J.; Bureau, Martin; Harrison, C. M.; Jarvis, Matt J.; Sharples, R. M.; Smail, Ian; Sobral, David; Best, P. N.; Cirasuolo, M.

doi:10.1093/mnras/stw129

Cited by 192 publications

(254 citation statements)

References 106 publications

Supporting

Mentioning

231

Contrasting

Order By: Relevance

“…The fraction of non-regular rotators found in the qmanga-galex sample (20%) is slightly higher than that found by previous works (14 − 17% of early-types in the ATLAS 3D sample; Emsellem et al 2011;Stott et al 2016). However, we must be wary with this comparison since the ATLAS 3D sample is volume limited, whereas the MaNGA sample is selected to have a flat stellar mass distribution, prior to our selection on GALEX cross-matches and those galaxies below the SFS.…”

Section: Identifying Slow and Fast Rotatorscontrasting

confidence: 69%

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

Smethurst

Masters

Lintott

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

Do the theorised different formation mechanisms of fast and slow rotators produce an observable difference in their star formation histories? To study this we identify quenching slow rotators in the MaNGA sample by selecting those which lie below the star forming sequence and identify a sample of quenching fast rotators which were matched in stellar mass. This results in a total sample of 194 kinematically classified galaxies, which is agnostic to visual morphology. We use u − r and N U V − u colours from SDSS and GALEX and an existing inference package, starpy, to conduct a first look at the onset time and exponentially declining rate of quenching of these galaxies. An Anderson-Darling test on the distribution of the inferred quenching rates across the two kinematic populations reveals they are statistically distinguishable (3.2σ). We find that fast rotators quench at a much wider range of rates than slow rotators, consistent with a wide variety of physical processes such as secular evolution, minor mergers, gas accretion and environmentally driven mechanisms. Quenching is more likely to occur at rapid rates (τ ∼ < 1 Gyr) for slow rotators, in agreement with theories suggesting slow rotators are formed in dynamically fast processes, such as major mergers. Interestingly, we also find that a subset of the fast rotators quench at these same rapid rates as the bulk of the slow rotator sample. We therefore discuss how the total gas mass of a merger, rather than the merger mass ratio, may decide a galaxy's ultimate kinematic fate.

show abstract

Section: Identifying Slow and Fast Rotatorscontrasting

confidence: 69%

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

Smethurst

Masters

Lintott

et al. 2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

show abstract

“…If the galaxies investigated here were to follow this constant halo-baryon fraction, the amount of missing gas-mass in the lowest mass galaxies (M * ≈ 10 8−9 M⊙), would be a factor of 20-10. While the amount of gas present in these star-forming galaxies may be significant compared to their stellar masses, such a high factor is larger than inferred for lowmass galaxies (M * < 10 10 M⊙) at z ∼ 1, which have gas masses of a factor of ∼2 larger than their stellar masses (Stott et al 2016). While some galaxies, particularly at z > 3, lie significantly below the z ∼ 1 stellar-mass TFR, most galaxies exhibit a spread around the relation with objects both above and below the relation.…”

Section: Intepretations Of a Break In The Tfrmentioning

confidence: 78%

A break in the high-redshift stellar mass Tully–Fisher relation

Christensen¹,

Hjorth²

2017

Monthly Notices of the Royal Astronomical Society

View full text Add to dashboard Cite

We investigate the stellar-mass Tully-Fisher relation (TFR) between the stellar mass and the integrated gas velocity dispersion, quantified by the kinematic estimator S 0.5 measured from strong emission lines in spectra of galaxies at 0 < z < 5. We combine luminosity-selected galaxies ('high-luminosity sample') with galaxies selected in other ways ('low-luminosity sample') to cover a range in stellar mass that spans almost five orders of magnitude: 7.0 ∼ < log M * /M ⊙ ∼ < 11.5. We find that the logarithmic power-law slope and normalisation of the TFR are independent of redshift out to z ∼ 3. The scatter in the TFR is < 0.5 dex such that the gas velocity dispersion can be used as a proxy for the stellar mass of a galaxy independently of its redshift. At z > 3 the scatter increases and the existence of a correlation is not obvious. The high-luminosity sample exhibits a flatter slope of 1.5±0.2 at z < 3 compared to the lowluminosity sample slope of 2.9±0.3, suggesting a turnover in the TFR. The combined sample is well fit with a break in the TFR at a characteristic stellar mass scale of M * ∼ 10 10 M ⊙ , with no significant evolution out to z ∼ 3. We demonstrate that a break in the TFR with a steeper slope at the low-mass end is a natural consequence of galaxy models with a mass-dependent stellar to halo-mass ratio.

show abstract

“…Significant progress in directly imaging the distribution of star formation at z>1 has been made with spatially resolved Hα spectroscopy, e.g., SINS (Förster Schreiber et al 2009), KMOS 3D (Wisnioski et al 2015), and KROSS (Stott et al 2016). Average Hα maps from 3D-HST, the largest sample thus far of resolved star formation at z=1.5-2.5, show that the star formation surface density, S SFR , on average peaks near the centers of massive galaxies (Nelson et al 2015).…”

Section: Introductionmentioning

confidence: 99%

VLA AND ALMA IMAGING OF INTENSE GALAXY-WIDE STAR FORMATION IN z ∼ 2 GALAXIES

Rujopakarn

Dunlop

Rieke

et al. 2016

ApJ

Self Cite

139

198

View full text Add to dashboard Cite

The full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-prot purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe present ;0 4 resolution extinction-independent distributions of star formation and dust in 11 star-forming galaxies (SFGs) at z=1.3-3.0. These galaxies are selected from sensitive blank-field surveys of the 2′×2′ Hubble Ultra-Deep Field at λ=5 cm and 1.3 mm using the Karl G. Jansky Very Large Array and Atacama Large Millimeter/submillimeter Array. They have star formation rates (SFRs), stellar masses, and dust properties representative of massive main-sequence SFGs at z∼2. Morphological classification performed on spatially resolved stellar mass maps indicates a mixture of disk and morphologically disturbed systems; half of the sample harbor X-ray active galactic nuclei (AGNs), thereby representing a diversity of z∼2 SFGs undergoing vigorous mass assembly. We find that their intense star formation most frequently occurs at the location of stellar-mass concentration and extends over an area comparable to their stellar-mass distribution, with a median diameter of 4.2±1.8 kpc. This provides direct evidence of galaxy-wide star formation in distant blank-field-selected mainsequence SFGs. The typical galactic-average SFR surface density is 2.5 M e yr −1 kpc −2 , sufficiently high to drive outflows. In X-ray-selected AGN where radio emission is enhanced over the level associated with star formation, the radio excess pinpoints the AGNs, which are found to be cospatial with star formation. The median extinctionindependent size of main-sequence SFGs is two times larger than those of bright submillimeter galaxies, whose SFRs are 3-8 times larger, providing a constraint on the characteristic SFR (∼300 M e yr −1 ) above which a significant population of more compact SFGs appears to emerge.

show abstract

The KMOS Redshift One Spectroscopic Survey (KROSS): dynamical properties, gas and dark matter fractions of typicalz∼ 1 star-forming galaxies

Cited by 192 publications

References 106 publications

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

A break in the high-redshift stellar mass Tully–Fisher relation

VLA AND ALMA IMAGING OF INTENSE GALAXY-WIDE STAR FORMATION IN z ∼ 2 GALAXIES

Contact Info

Product

Resources

About