Do Galaxy Morphologies Really Affect the Efficiency of Star Formation During the Phase of Galaxy Transition?

Koyama, Shuhei; Koyama, Yusei; Yamashita, Takuji; Hayashi, Masao; Matsuhara, Hideo; Namiki, Shigeru V.; Suzuki, Tomoko L.; Fukagawa, Nao; Kodama, Tadayuki; Lin, Lihwai; Morokuma-Matsui, Kana; Shimakawa, Rhythm; Tanaka, Ichi

doi:10.3847/1538-4357/ab0e75

Cited by 18 publications

(15 citation statements)

References 54 publications

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“…We consider that the transition from one spiral pattern (ordered state) to another via gas ejection (disordered state) from the central star would be related to chaotic itinerancy [1,20] in high-dimensional dynamical systems [4,21,22]. Moreover, we expect that the evolution from spiral patterns to less sharp patterns in the transition would be concerned with the evolution from starforming spiral galaxies to non-star-forming elliptical galaxies, which is called galaxy "quenching" [23,24]. These will be reported elsewhere.…”

Section: Summary and Discussionmentioning

confidence: 99%

Coupled map lattice for the spiral pattern formation in astronomical objects

Nozawa

2020

Physica D: Nonlinear Phenomena

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We propose a minimal coupled map lattice (CML) for the spiral pattern formation in astronomical objects which consist of accreting gas induced by gravity as a long-range force. In the proposed CML, we assume only two procedures: one in which the flow of gas particles occurs by gravity and another one in which the collision of gas particles occurs by advection in the flow. In spite of its simplicity, the numerical simulation of the proposed CML shows a new formation process in which grand design spiral patterns appear due to gas ejection from a central star. Several aspects of the formation process are indeed in good agreement with the results of conventional theories and observations. This agreement and the observations of outflows should suggest that the above gas ejection can happen and lead to the formation of grand design spiral patterns, in actual spiral galaxies and protoplanetary disks.

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Section: Summary and Discussionmentioning

confidence: 99%

Coupled map lattice for the spiral pattern formation in astronomical objects

Nozawa

2020

Physica D: Nonlinear Phenomena

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“…González Delgado et al 2016), galaxy morphology and structural properties seem to play a role in modifying the SFE. On average, τ dep,mol appears to decrease moving from early-to late-type systems (Colombo et al 2018), following the decrease in shear (Davis et al 2014;Colombo et al 2018) as described by the morphological quenching scenario (however, see Koyama et al 2019). The molecular depletion time is also seen to decrease with stellar surface density and increase with molecular gas velocity dispersion (Dey et al 2019).…”

Section: Introductionmentioning

confidence: 88%

The EDGE-CALIFA survey: exploring the role of molecular gas on galaxy star formation quenching

Colombo

Sanchez

Bolatto

et al. 2020

A&A

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Understanding how galaxies cease to form stars represents an outstanding challenge for galaxy evolution theories. This process of "star formation quenching" has been related to various causes, including active galactic nuclei activity, the influence of large-scale dynamics, and the environment in which galaxies live. In this paper, we present the first results from a follow-up of CALIFA survey galaxies with observations of molecular gas obtained with the APEX telescope. Together with the EDGE-CARMA observations, we collected 12 CO observations that cover approximately one effective radius in 472 CALIFA galaxies. We observe that the deficit of galaxy star formation with respect to the star formation main sequence (SFMS) increases with the absence of molecular gas and with a reduced efficiency of conversion of molecular gas into stars, which is in line with the results of other integrated studies. However, by dividing the sample into galaxies dominated by star formation and galaxies quenched in their centres (as indicated by the average value of the Hα equivalent width), we find that this deficit increases sharply once a certain level of gas consumption is reached, indicating that different mechanisms drive separation from the SFMS in star-forming and quenched galaxies. Our results indicate that differences in the amount of molecular gas at a fixed stellar mass are the primary drivers for the dispersion in the SFMS, and the most likely explanation for the start of star formation quenching. However, once a galaxy is quenched, changes in star formation efficiency drive how much a retired galaxy differs in its star formation rate from star-forming ones of similar masses. In other words, once a paucity of molecular gas has significantly reduced star formation, changes in the star formation efficiency are what drives a galaxy deeper into the red cloud, hence retiring it.

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“…Although here the star formation per unit gas mass is reduced with respect to that observed in gas-rich, rotating spirals, the amount of star formed per freefall time is constant (Davis et al 2014). This result might be tightly connected to the more general "morphological quenching" scenario proposed by Martig et al (2009), where gas discs can be stabilised against star formation when they are embedded in prominent bulges such as those observed in lenticular galaxies (see however Koyama et al 2019). Although our re-sults are in line with these interpretations, we caution that both the star formation rates and the molecular gas column densities used in Fig.…”

Section: Schmidt Relationmentioning

confidence: 66%

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE).XII. Ionised gas emission in the inner regions of lenticular galaxies

Boselli,

Fossati,

Longobardi

et al. 2021

Preprint

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As part of the Virgo Cluster Survey Tracing Ionised Gas Emission (VESTIGE), a blind narrow-band Hα+ [NII] imaging survey of the Virgo cluster carried out with MegaCam at the CFHT, we discovered eight massive (10 10 M star 10 11 M ) lenticular galaxies with prominent ionised gas emission features in their inner (few kpc) regions. These features are either ionised gas filaments similar to those observed in cooling flows (2 galaxies), or thin discs with sizes 0.7 R(Hα) 2.0 kpc (6 galaxies), thus significantly smaller than those of the stellar disc (R(Hα) 7-22 % R iso (r)). These discs have morphological properties similar to those of the dust seen in absorption in high-resolution HST images. Using a unique set of multifrequency data, including new or archival ASTROSAT/UVIT, GALEX, HST, CFHT, Spitzer, and Herschel imaging data, combined with IFU (MUSE, ALMA) and long-slit (SOAR) spectroscopy, we show that while the gas located within these inner discs is photoionised by young stars, signaling ongoing star formation, the gas in the filamentary structures is shock-ionised. These discs have a star formation surface brightness similar to those observed in late-type galaxies. Because of their reduced size, however, these lenticular galaxies are located below the main sequence of unperturbed or cluster star-forming systems. By comparing the dust masses measured from absorption maps in optical images, from the Balmer decrement, or estimated by fitting the UV-to-far-IR spectral energy distribution of the target galaxies, we confirm that those derived from optical attenuation maps are heavily underestimated because of geometrical effects due to the relative distribution of the absorbing dust and the emitting stars. We have also shown that these galaxies have gas-to-dust ratios of G/D 80 320 30 , and that the star formation within these discs follows the Schmidt relation, albeit with an efficiency reduced by a factor of ∼ 2.5. Using our unique set of multifrequency data, we discuss the possible origin of the ionised gas in these objects, which suggests multiple and complex formation scenarios for massive lenticular galaxies in clusters.

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Do Galaxy Morphologies Really Affect the Efficiency of Star Formation During the Phase of Galaxy Transition?

Cited by 18 publications

References 54 publications

Coupled map lattice for the spiral pattern formation in astronomical objects

Coupled map lattice for the spiral pattern formation in astronomical objects

The EDGE-CALIFA survey: exploring the role of molecular gas on galaxy star formation quenching

A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE).XII. Ionised gas emission in the inner regions of lenticular galaxies

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