A multiscale study of star formation in Messier 33

Elson, Ed; Kam, Sié; Chemin, L.; Carignan, C.; Jarrett, T. H.

doi:10.1093/mnras/sty3091

Cited by 12 publications

(12 citation statements)

References 47 publications

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“…Williams et al (2018) derived a SFR of 0.25 +0.01 −0.07 M yr −1 using the FUV+24 µm method (Leroy et al 2008) and 0.33 +0.05 −0.06 M yr −1 from a global fit and the MAGPHYS code (Da Cunha et al 2008). Elson et al (2019) derive a SFR of 0.34 +0.08 −0.07 M yr −1 using 12 µm estimates and the calibrated global WISE W3 luminosities to SFRs presented in Cluver et al (2017), and (0.44 ± 0.10) M yr −1 , based on the linear relation between 100 µm emission and total SFR presented by Boquien et al (2010).…”

Section: Star-formation Ratementioning

confidence: 99%

A radiative transfer model for the spiral galaxy M33★

Thirlwall

Popescu

Tuffs

et al. 2020

Monthly Notices of the Royal Astronomical Society

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We present the first radiative transfer (RT) model of a non-edge-on disk galaxy in which the large-scale geometry of stars and dust is self-consistently derived through fitting of multiwavelength imaging observations from the UV to the submm. To this end we used the axi-symmetric RT model of Popescu et al. and a new methodology for deriving geometrical parameters, and applied this to decode the spectral energy distribution (SED) of M33. We successfully account for both the spatial and spectral energy distribution, with residuals typically within 7% in the profiles of surface brightness and within 8% in the spatially-integrated SED. We predict well the energy balance between absorption and re-emission by dust, with no need to invoke modified grain properties, and we find no submm emission that is in excess of our model predictions. We calculate that 80 ± 8% of the dust heating is powered by the young stellar populations. We identify several morphological components in M33, a nuclear, an inner, a main and an outer disc, showing a monotonic trend in decreasing star-formation surface-density (Σ SFR ) from the nuclear to the outer disc. In relation to surface density of stellar mass, the Σ SFR of these components define a steeper relation than the "main sequence" of star-forming galaxies, which we call a "structurally resolved main sequence". Either environmental or stellar feedback mechanisms could explain the slope of the newly defined sequence. We find the star-formation rate to be SFR = 0.28 +0.02 −0.01 M yr −1 .

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Section: Star-formation Ratementioning

confidence: 99%

A radiative transfer model for the spiral galaxy M33★

Thirlwall

Popescu

Tuffs

et al. 2020

Monthly Notices of the Royal Astronomical Society

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“…Approaching the excellent spatial resolution (∼18 pc) of the ALMA maps for the SFR is not possible, but the use of the 8 μm instead of 24 μm emission to trace the SFR mitigates this issue by a factor of 2 (Maragkoudakis et al 2017), and so we chose the 8 μm band for our analysis because of its higher angular resolution (2 4, or 43 pc) compared to that of the 24 μm data (6 0, or 108 pc). Moreover, Elson et al (2019) showed that the 8 μm PAH emission is a robust SFR tracer down to physical spatial resolutions of 49 pc. PAH emission represents generally more than 70% of the 8 μm emission (Calzetti 2011) and dominates by more than a factor of 100 above the warm dust emission and about a factor of 5 above the stellar continuum (Li & Draine 2001;Dale et al 2005;Young et al 2014a).…”

Section: Validity Of Using 8 μM Pah Data As Star Formation Rate Tracermentioning

confidence: 99%

“…PAH emission represents generally more than 70% of the 8 μm emission (Calzetti 2011) and dominates by more than a factor of 100 above the warm dust emission and about a factor of 5 above the stellar continuum (Li & Draine 2001;Dale et al 2005;Young et al 2014a). As a consequence, PAH emission (and in particular from the Spitzer 8 μm band) has been used in the literature to estimate SFR in galaxies (Calzetti et al 2005;Wu et al 2005;Pérez-González et al 2006;Zhu et al 2008;Pancoast et al 2010;Calzetti 2011;Kennicutt & Evans 2012;Young et al 2014a;Cluver et al 2017;Kokusho et al 2017;Maragkoudakis et al 2017;Hall et al 2018;Elson et al 2019;Mahajan et al 2019). Nevertheless, there may be variations from galaxy to galaxy, due to metallicity or different beam filling factors (Calzetti et al 2005;Engelbracht et al 2005;Pérez-González et al 2006;Young et al 2014a), so it is necessary to assess the validity of the 8 μm PAH emission as a reliable SF tracer in Cen A.…”

Section: Validity Of Using 8 μM Pah Data As Star Formation Rate Tracermentioning

confidence: 99%

Star Formation Efficiencies at Giant Molecular Cloud Scales in the Molecular Disk of the Elliptical Galaxy NGC 5128 (Centaurus A)

Espada

Verley

Miura

et al. 2019

ApJ

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We present ALMA CO (1−0) observations toward the dust lane of the nearest elliptical and radio galaxy, NGC 5128 (Centaurus A), with high angular resolution (∼1″, or 18 pc), including information from large to small spatial scales and total flux. We find a total molecular gas mass of 1.6×10 9 M e and reveal the presence of filamentary components more extended than previously seen, up to a radius of 4 kpc. We find that the global star formation rate is ∼1 M e yr −1 , which yields a star formation efficiency (SFE) of 0.6 Gyr −1 (depletion time τ=1.5 Gyr), similar to those in disk galaxies. We show the most detailed view to date (40 pc resolution) of the relation between molecular gas and star formation within the stellar component of an elliptical galaxy, from a scale of several kiloparsecs to the circumnuclear region close to the powerful radio jet. Although on average the SFEs are similar to those of spiral galaxies, the circumnuclear disk (CND) presents SFEs of 0.3 Gyr −1 , lower by a factor of 4 than the outer disk. The low SFE in the CND is in contrast to the high SFEs found in the literature for the circumnuclear regions of some nearby disk galaxies with nuclear activity, probably as a result of larger shear motions and longer active galactic nucleus feedback. The higher SFEs in the outer disk suggest that only central molecular gas or filaments with sufficient density and strong shear motions will remain in ∼1 Gyr, which will later result in the compact molecular distributions and low SFEs usually seen in other giant ellipticals with cold gas.

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“…Some examples include studies based on The H i Nearby Galaxy Survey (THINGS, Walter et al 2008) and its data (Bigiel et al 2008;Leroy et al 2008). Other recent works include Zheng et al (2013) on the regulation of star formation; as well as Thilker et al (2007) and Holwerda et al (2012) on the link between star formation and H i morphology (implying a physical link; Heiner et al 2008); studies of multi-scale star formation and H i (Elson et al 2019); the link between SFR and gas based on jellyfish galaxies (Jáchym et al 2019;Ramatsoku et al 2019Ramatsoku et al , 2020Moretti et al 2020); and Bacchini et al (2019) on the link between SFR and H i volume densities.…”

Section: Introductionmentioning

confidence: 99%

MeerKAT HI commissioning observations of MHONGOOSE galaxy ESO 302-G014

Blok

Athanassoula

Bosma

et al. 2020

A&A

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Aims. We present the results of three commissioning H I observations obtained with the MeerKAT radio telescope. These observations make up part of the preparation for the forthcoming MHONGOOSE nearby galaxy survey, which is a MeerKAT large survey project that will study the accretion of gas in galaxies and the link between gas and star formation. Methods. We used the available H I data sets, along with ancillary data at other wavelengths, to study the morphology of the MHONGOOSE sample galaxy, ESO 302-G014, which is a nearby gas-rich dwarf galaxy. Results. We find that ESO 302-G014 has a lopsided, asymmetric outer disc with a low column density. In addition, we find a tail or filament of H I clouds extending away from the galaxy, as well as an isolated H I cloud some 20 kpc to the south of the galaxy. We suggest that these features indicate a minor interaction with a low-mass galaxy. Optical imaging shows a possible dwarf galaxy near the tail, but based on the current data, we cannot confirm any association with ESO 302-G014. Nonetheless, an interaction scenario with some kind of low-mass companion is still supported by the presence of a significant amount of molecular gas, which is almost equal to the stellar mass, and a number of prominent stellar clusters, which suggest recently triggered star formation. Conclusions. These data show that MeerKAT produces exquisite imaging data. The forthcoming full-depth survey observations of ESO 302-G014 and other sample galaxies will, therefore, offer insights into the fate of neutral gas as it moves from the intergalactic medium onto galaxies.

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A multiscale study of star formation in Messier 33

Cited by 12 publications

References 47 publications

A radiative transfer model for the spiral galaxy M33★

A radiative transfer model for the spiral galaxy M33★

Star Formation Efficiencies at Giant Molecular Cloud Scales in the Molecular Disk of the Elliptical Galaxy NGC 5128 (Centaurus A)

MeerKAT HI commissioning observations of MHONGOOSE galaxy ESO 302-G014

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