STAR FORMATION RATE IN LATE-TYPE GALAXIES: I- THE Hα AND FUV INTEGRATED VALUES

Serrano, Moises; Gamez, Ana María Hidalgo; Vega-Acevedo, I.; Castañeda, H. O.

doi:10.22201/ia.01851101p.2020.56.01.06

Cited by 6 publications

(6 citation statements)

References 70 publications

(107 reference statements)

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“…. This assumption agrees with the conclusion of [4], where the authors, based on a small sample of late-type galaxies (14 dS and 22 Sm) inferred that "dS are forming a larger number of stars per area than Sm, despite the fact that the latter on average has twice more gas mass than dS."…”

Section: Discussionsupporting

confidence: 89%

“…A more detailed comparison of star formation rate of dwarf galaxies possessing spiral arms (dS) and without spirals (Sm) was presented by [4]. There the authors concluded that Sm galaxies have higher star formation rate values (SFR) than dS, however when the surface density of SFR is considered, both types of galaxies are indistinguishable.…”

Section: Introductionmentioning

confidence: 99%

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On the Formation of Spiral Arms in Dwarf Galaxies

et al. 2021

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Spiral structure (both flocculent and Grand Design types) is very rarely observed in dwarf galaxies because the formation of spiral arms requires special conditions. In this work we analyze the sample of about 40 dS-galaxies found by scanning by eye the images of late-type galaxies with and and photometric diameter kpc. We found that apart from the lower average gas (HI) fraction the other properties of dS-galaxies including the presence of a bar and the isolation index do not differ much from those for dwarf Irr or Sm-types of similar luminosity and rotation velocity (or specific angular momentum).There are practically no dS-galaxies with rotation velocity below 50-60 km s -1 . To check the conditions of formation of spiral structure in dwarf galaxies we carried out a series of N-body/hydrodynamic simulations of lowmass stellar-gaseous discy galaxies by varying the model kinematic parameters of discs, their initial thickness, relative masses and scale lengths of stellar and gaseous disc components, and stellar-to-dark halo masses. We came to conclusion that the gravitational mechanism of spiral structure formation is effective only for thin stellar discs, which are non-typical for dwarf galaxies, and for not too slowly rotating galaxies. Therefore, only a small fraction of dwarf galaxies with stellar/gaseous discs have spiral or ring structures. The thicker stellar disc, the more gas is required for the spiral structure to form. The reduced gas content in many dS-galaxies compared to non-spiral ones may be a result of more efficient star formation due to a higher volume gas density thank to the thinner stellar/gaseous discs.

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Section: Discussionsupporting

confidence: 89%

Section: Introductionmentioning

confidence: 99%

On the Formation of Spiral Arms in Dwarf Galaxies

et al. 2021

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“…Increasing the SFR in a galaxy speeds up the rate of gas consumption, thereby facilitating the transition from star forming to quenched. An increase in SFR in barred galaxies has been observed before (Alonso-Herrero & Knapen 2001;Hunt et al 2008;Ellison et al 2011;Coelho & Gadotti 2011;Hirota et al 2014;Janowiecki et al 2020;Magaña-Serrano et al 2020;Lin et al 2020). However, we conclude that, on average, only strong bars in SF galaxies help to quench their host through secular evolution.…”

Section: Strong Bars In Star Forming Galaxies Facilitate Quenchingsupporting

confidence: 49%

“…The simulations of Athanassoula et al (2013) have demonstrated that bars tend to form later if the gas fraction is high. Some observations show higher SFE/SFR in barred regions (Alonso-Herrero & Knapen 2001;Hunt et al 2008;Coelho & Gadotti 2011;Hirota et al 2014;Janowiecki et al 2020;Magaña-Serrano et al 2020;Lin et al 2020), while others observe lower SFR/SFE (Momose et al 2010;Yajima et al 2019;Maeda et al 2020). Sheth et al (2000) has shown a lower SFR in the region between the centre and bar ends, but higher in the very centre.…”

Section: Introductionmentioning

confidence: 96%

Galaxy Zoo: Stronger bars facilitate quenching in star forming galaxies

Géron,

Smethurst,

Lintott

et al. 2021

Preprint

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We have used Galaxy Zoo DECaLS (GZD) to study strong and weak bars in disk galaxies. Out of the 314,000 galaxies in GZD, we created a volume-limited sample (0.01 < z < 0.05, 𝑀 r < −18.96) which contains 1,867 galaxies with reliable volunteer bar classifications in the ALFALFA footprint. In keeping with previous Galaxy Zoo surveys (such as GZ2), the morphological classifications from GZD agree well with previous morphological surveys. GZD considers galaxies to either have a strong bar (15.5%), a weak bar (28.1%) or no bar (56.4%), based on volunteer classifications on images obtained from the DECaLS survey. This places GZD in a unique position to assess differences between strong and weak bars. We find that the strong bar fraction is typically higher in quiescent galaxies than in star forming galaxies, while the weak bar fraction is similar. Moreover, we have found that strong bars facilitate the quenching process in star forming galaxies, finding higher fibre SFRs, lower gas masses and shorter depletion timescales in these galaxies compared to unbarred galaxies. However, we also found that any differences between strong and weak bars disappear when controlling for bar length. Based on this, we conclude that weak and strong bars are not fundamentally different phenomena. Instead, we propose that there is a continuum of bar types, which varies from 'weakest' to 'strongest'.

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“…A more detailed comparison of star formation rate of dwarf galaxies possessing spiral arms (dS) and without spirals (Sm) was presented by Magaña-Serrano et al (2020). They concluded that Sm galaxies have higher star formation rate values (SFR) than dS, however when the surface density of SFR is considered, both types of galaxies are indistinguishable.…”

mentioning

confidence: 99%

On the formation of spiral arms in dwarf galaxies

Zasov,

Khoperskov,

Zaitseva

et al. 2021

Preprint

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Spiral structure (both flocculent and Grand Design types) is very rarely observed in dwarf galaxies because the formation of spiral arms requires special conditions. In this work we analyze the sample of about 40 dS-galaxies found by scanning by eye the images of late-type galaxies with 𝑚 𝐵 < 15 𝑚 and 𝑀 𝐵 > −18 𝑚 and photometric diameter 𝐷 25 < 12 kpc. We found that apart from the lower average gas (HI) fraction the other properties of dS-galaxies including the presence of a bar and the isolation index do not differ much from those for dwarf Irr or Sm-types of similar luminosity and rotation velocity (or specific angular momentum).There are practically no dS-galaxies with rotation velocity below 50 -60 km sec −1 .To check the conditions of formation of spiral structure in dwarf galaxies we carried out a series of N-body/hydrodynamic simulations of low-mass stellar-gaseous discy galaxies by varying the model kinematic parameters of discs, their initial thickness, relative masses and scale lengths of stellar and gaseous disc components, and stellar-to-dark halo masses. We came to conclusion that the gravitational mechanism of spiral structure formation is effective only for thin stellar discs, which are non-typical for dwarf galaxies, and for not too slowly rotating galaxies. Therefore, only a small fraction of dwarf galaxies with stellar/gaseous discs have spiral or ring structures. The thicker stellar disc, the more gas is required for the spiral structure to form. The reduced gas content in many dS-galaxies compared to non-spiral ones may be a result of more efficient star formation due to a higher volume gas density thank to the thinner stellar/gaseous discs.

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STAR FORMATION RATE IN LATE-TYPE GALAXIES: I- THE Hα AND FUV INTEGRATED VALUES

Cited by 6 publications

References 70 publications

On the Formation of Spiral Arms in Dwarf Galaxies

On the Formation of Spiral Arms in Dwarf Galaxies

Galaxy Zoo: Stronger bars facilitate quenching in star forming galaxies

On the formation of spiral arms in dwarf galaxies

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