The
                    <i>GALEX</i>
                    Ultraviolet Atlas of Nearby Galaxies

Paz, A. Gil de; Boissier, S.; Madore, Barry F.; Seibert, Mark; Joe, Yung Il; Boselli, A.; Wyder, Ted K.; Thilker, David A.; Bianchi, Luciana; Rey, Soo-Chang; Rich, R. Michael; Barlow, Tom A.; Conrow, T.; Forster, Karl; Friedman, Peter G.; Martin, D. Christopher; Morrissey, Patrick; Neff, Susan G.; Schiminovich, David; Small, Todd; Donas, J.; Heckman, Timothy M.; Lee, Young-Wook; Milliard, B.; Szalay, Alexander S.; Yi, Sukyoung K.

doi:10.1086/516636

Cited by 737 publications

(671 citation statements)

References 121 publications

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“…To account molecule photodestruction we should know spatial structure of UV background in the galactic disc. Recent observations provide some evidences for significant radial and azimuthal variations of UV flux in the nearby galaxies (Gil de Paz et al 2007). No doubt that such variations are stipulated by local star formation.…”

Section: Modelmentioning

confidence: 96%

A Kennicutt–Schmidt relation at molecular cloud scales and beyond

Khoperskov

Vasiliev

2017

Monthly Notices of the Royal Astronomical Society

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Using N -body/gasdynamic simulations of a Milky Way-like galaxy we analyse a Kennicutt-Schmidt relation, Σ SFR ∝ Σ gas N , at different spatial scales. We simulate synthetic observations in CO lines and UV band. We adopt the star formation rate (SFR) defined in two ways: based on free fall collapse of a molecular cloud -Σ SFR, cl , and calculated by using a UV flux calibration -Σ SFR, UV . We study a KS relation for spatially smoothed maps with effective spatial resolution from molecular cloud scales to several hundred parsecs. We find that for spatially and kinematically resolved molecular clouds the Σ SFR, cl ∝ Σ gas N relation follows the power-law with index N ≈ 1.4. Using UV flux as SFR calibrator we confirm a systematic offset between the Σ SFR, UV and Σ gas distributions on scales compared to molecular cloud sizes. Degrading resolution of our simulated maps for surface densities of gas and star formation rates we establish that there is no relation Σ SFR, UV − Σ gas below the resolution ∼ 50 pc. We find a transition range around scales ∼ 50 − 120 pc, where the power-law index N increases from 0 to 1 − 1.8 and saturates for scales larger ∼ 120 pc. A value of the index saturated depends on a surface gas density threshold and it becomes steeper for higher Σ gas threshold. Averaging over scales with size of > ∼ 150 pc the power-law index N equals 1.3 − 1.4 for surface gas density threshold ∼ 5 M ⊙ pc −2 . At scales > ∼ 120 pc surface SFR densities determined by using CO data and UV flux, Σ SFR, UV /Σ SFR, cl , demonstrate a discrepancy about a factor of 3. We argue that this may be originated from overestimating (constant) values of conversion factor, star formation efficiency or UV calibration used in our analysis.

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Section: Modelmentioning

confidence: 96%

A Kennicutt–Schmidt relation at molecular cloud scales and beyond

Khoperskov

Vasiliev

2017

Monthly Notices of the Royal Astronomical Society

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“…The green dashed line at 8.8 mag defines the separation between star-forming and non-star-forming as per Gil de Paz et al (2007). The galaxies are color coded to represent the strength of the radio power.…”

Section: Sfr Estimation Using Fuvmentioning

confidence: 99%

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

Vaddi

O’Dea

Baum

et al. 2016

ApJ

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We address the relation between star formation and active galactic nucleus (AGN) activity in a sample of 231 nearby (0.0002 < z < 0.0358) early-type galaxies by carrying out a multi-wavelength study using archival observations in the UV, IR, and radio. Our results indicate that early-type galaxies in the current epoch are rarely powerful AGNs, with P 10 WHz 22 1 < -for a majority of the galaxies. Only massive galaxies are capable of hosting powerful radio sources while less massive galaxies are hosts to lower radio power sources. Evidence of ongoing star formation is seen in approximately 7% of the sample. The star formation rate (SFR) of these galaxies is less than 0.1 M e yr −1 . They also tend to be radio faint (P 10 WHzThere is a nearly equal fraction of star-forming galaxies in radio faint (P 10 WHz 22 1 < -) and radio bright galaxies (P 10 WHz 22 1  -) suggesting that both star formation and radio mode feedback are constrained to be very low in our sample. We notice that our galaxy sample and the Brightest Cluster Galaxies follow similar trends in radio power versus SFR. This may be produced if both radio power and SFR are related to stellar mass.

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“…Here, the integral SFR of a galaxy is usually estimated either by the integral flux in the emission Hα line, or by the flux in the far ultraviolet (F U V ), measured by GALEX satellite (Gil de Paz, 2007). reviewed the data available in the UNGC catalog on star formation rates in galaxies of the Local Volume depending on their tidal index Θ 1 .…”

Section: Hi-richness In Population Of the Nearby Groupsmentioning

confidence: 99%

Companions around the nearest luminous galaxies: Segregation and selection effects

Караченцев

Kudrya

2015

Astron Nachr

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Using the "Updated Nearby Galaxy Catalog", we consider different properties of companion galaxies around luminous hosts in the Local Volume. The data on stellar masses, linear diameters, surface brightnesses, HI-richness, specific star formation rate (sSF R), and morphological types are discussed for members of the nearest groups, including the Milky Way and M 31 groups, as a function of their separation from the hosts. Companion galaxies in groups tend to have lower stellar masses, smaller linear diameters and fainter mean surface brightnesses as the distance to their host decreases. The hydrogen-to-stellar mass ratio of the companions increases with their linear projected separation from the dominant luminous galaxy. This tendency is more expressed around the bulge-dominated hosts. While linear separation of the companions decreases, their mean sSF R becomes lower, accompanied with the increasing sSF R scatter. Typical linear projected separation of dSphs around the bulge-dominated hosts, 350 kpc, is substantially larger than that around the disk-dominated ones, 130 kpc. This difference probably indicates the presence of larger hot/warm gas haloes around the early-type host galaxies. The mean fraction of dSph (quenched) companions in 11 the nearest groups as a function of their projected separation Rp can be expressed as f (E) = 0.55 − 0.69 × Rp. The fraction of dSphs around the Milky Way and M 31 looks much higher than in other nearby groups because the quenching efficiency dramatically increases towards the ultra-low mass companions. We emphasize that the observed properties of the Local Group are not typical for other groups in the Local Volume due to the role of selection effects caused by our location inside the Local Group.

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The GALEX Ultraviolet Atlas of Nearby Galaxies

Cited by 737 publications

References 121 publications

A Kennicutt–Schmidt relation at molecular cloud scales and beyond

A Kennicutt–Schmidt relation at molecular cloud scales and beyond

Constraints on Feedback in the Local Universe: The Relation Between Star Formation and Agn Activity in Early-Type Galaxies

Companions around the nearest luminous galaxies: Segregation and selection effects

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