An ALMA/HST Study of Millimeter Dust Emission and Star Clusters

Turner, Jordan A.; Dale, Daniel A.; Adamo, Angela; Calzetti, Daniela; Grasha, Kathryn; Grebel, Eva K.; Johnson, K. E.; Lee, Janice; Smith, Linda J.; Yoon, Ilsang

doi:10.3847/1538-4357/ab3faa

Cited by 3 publications

(3 citation statements)

References 32 publications

(40 reference statements)

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“…It was observed by the LEGUS survey with two pointings. This galaxy has been observed extensively by all recent major surveys of interstellar gas and dust in nearby galaxies, including THINGS, HERACLES, SINGS, KINGFISH, EMPIRE, and with ALMA (Kennicutt et al 2003(Kennicutt et al , 2011Walter et al 2008;Leroy et al 2009;Bigiel et al 2016;Turner et al 2019). Elmegreen et al (2006) investigated hierarchical star formation in this galaxy, and Grasha et al (2015) report a measurement of its TPCF.…”

Section: Ngc 0628mentioning

confidence: 97%

The dependence of the hierarchical distribution of star clusters on galactic environment

Menon

Grasha

Elmegreen³

et al. 2021

Monthly Notices of the Royal Astronomical Society

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We use the angular Two Point Correlation Function (TPCF) to investigate the hierarchical distribution of young star clusters in 12 local (3–18 Mpc) star-forming galaxies using star cluster catalogues obtained with the Hubble Space Telescope (HST) as part of the Treasury Program LEGUS (Legacy ExtraGalactic UV Survey). The sample spans a range of different morphological types, allowing us to infer how the physical properties of the galaxy affect the spatial distribution of the clusters. We also prepare a range of physically motivated toy models to compare with and interpret the observed features in the TPCFs. We find that, conforming to earlier studies, young clusters (T ≲ 10 Myr) have power-law TPCFs that are characteristic of fractal distributions with a fractal dimension D2, and this scale-free nature extends out to a maximum scale lcorr beyond which the distribution becomes Poissonian. However, lcorr, and D2 vary significantly across the sample, and are correlated with a number of host galaxy physical properties, suggesting that there are physical differences in the underlying star cluster distributions. We also find that hierarchical structuring weakens with age, evidenced by flatter TPCFs for older clusters (T ≳ 10 Myr), that eventually converges to the residual correlation expected from a completely random large-scale radial distribution of clusters in the galaxy in ∼100 Myr. Our study demonstrates that the hierarchical distribution of star clusters evolves with age, and is strongly dependent on the properties of the host galaxy environment.

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Section: Ngc 0628mentioning

confidence: 97%

The dependence of the hierarchical distribution of star clusters on galactic environment

Menon

Grasha

Elmegreen³

et al. 2021

Monthly Notices of the Royal Astronomical Society

Self Cite

View full text Add to dashboard Cite

show abstract

“…It was observed by the LEGUS survey with two pointings. This galaxy has been observed extensively by all recent major surveys of interstellar gas and dust in nearby galaxies, including THINGS, HERACLES, SINGS, KINGFISH, EMPIRE, and with ALMA (Walter et al 2008;Leroy et al 2009;Kennicutt et al 2003Kennicutt et al , 2011Bigiel et al 2016;Turner et al 2019). Elmegreen et al (2006) investigated hierarchical star formation in this galaxy, and Grasha et al (2015) report a measurement of its TPCF.…”

Section: Ngc 0628mentioning

confidence: 96%

The Dependence of the Hierarchical Distribution of Star Clusters on Galactic Environment

Menon,

Grasha,

Elmegreen

et al. 2021

Preprint

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We use the angular Two Point Correlation Function (TPCF) to investigate the hierarchical distribution of young star clusters in 12 local (3-18 Mpc) star-forming galaxies using star cluster catalogues obtained with the Hubble Space Telescope (HST) as part of the Treasury Program LEGUS (Legacy ExtraGalactic UV Survey). The sample spans a range of different morphological types, allowing us to infer how the physical properties of the galaxy affect the spatial distribution of the clusters. We also prepare a range of physically motivated toy models to compare with and interpret the observed features in the TPCFs. We find that, conforming to earlier studies, young clusters (𝑇 < ∼ 10 Myr) have power-law TPCFs that are characteristic of fractal distributions with a fractal dimension 𝐷 2 , and this scale-free nature extends out to a maximum scale 𝑙 corr beyond which the distribution becomes Poissonian. However, 𝑙 corr , and 𝐷 2 vary significantly across the sample, and are correlated with a number of host galaxy physical properties, suggesting that there are physical differences in the underlying star cluster distributions. We also find that hierarchical structuring weakens with age, evidenced by flatter TPCFs for older clusters (𝑇 > ∼ 10 Myr), that eventually converges to the residual correlation expected from a completely random large-scale radial distribution of clusters in the galaxy in ∼ 100 Myr. Our study demonstrates that the hierarchical distribution of star clusters evolves with age, and is strongly dependent on the properties of the host galaxy environment.

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“…For example, the PHANGS Large Program demonstrated that the properties of molecular clouds on ∼100 pc scales correlate with their location in the host galaxy, with higher surface densities and turbulent pressure toward the center of galaxies and in spiral arms compared to interarm regions (Sun et al 2020;Leroy et al 2021). Detailed studies of the M33 and the Antennae galaxies (to name a few), have revealed that the large-scale filamentary structure of GMCs in the Milky Way is ubiquitous in both "normal" and starburst galaxies (Tokuda et al 2020;Whitmore et al 2014), while studies of numerous dwarf galaxies have begun to explore the consequences of low-metallicity star formation on chemical complexity (Shimonishi et al 2018;Turner et al 2019;Sewi lo et al 2022). Detailed studies of the nuclear regions of galaxies have also been obtained by ALMA to provide a global perspective on cloud properties (Costagliola et al 2015;Meier et al 2015;Harada et al 2018Harada et al , 2019Martín et al 2021;Sakamoto et al 2021a,b).…”

Section: Star Formationmentioning

confidence: 99%

The ALMA2030 Wideband Sensitivity Upgrade

Carpenter¹,

Brogan²,

Iono³

et al. 2022

Preprint

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The Wideband Sensitivity Upgrade (WSU) is the top priority initiative for the ALMA2030 Development Roadmap. The WSU will initially double, and eventually quadruple, ALMA's system bandwidth and will deliver improved sensitivity by upgrading the receivers, digital electronics, and correlator. The WSU will afford significant improvements for every future ALMA observation, whether it is focused on continuum or spectral line science. The continuum imaging speed will increase by at least a factor of 3 for the 2× bandwidth upgrade (and at least a factor of 6 for the 4× upgrade), plus any speed gains from improved receiver temperatures. The (single) spectral line imaging speed is expected to improve by a factor of 2-3 depending on the receiver band. The improvements provided by the WSU will be most dramatic for high spectral resolution observations, where the instantaneous bandwidth correlated at ∼ 0.1-0.2 km s −1 resolution will increase by 1-2 orders of magnitude in most receiver bands, with the largest gains at the lowest frequencies. The improved sensitivity and spectral tuning grasp will open new avenues of exploration, increase sample sizes, and enable more efficient observations. The impact will span the vast array of astronomical topics that embodies ALMA's motto In Search of our Cosmic Origins. The WSU will greatly expand the chemical inventory of protoplanetary disks that surround young stars, which will have profound implications for how and when planets form in disks and their composition. Observations of the interstellar medium in the Milky Way and nearby galaxies will simultaneously measure a variety of molecular species that will be used to build large samples of clouds, cores, and protostars in a variety of evolutionary states. The WSU will also enable efficient surveys of galaxies at high redshift to probe the origins of galaxies. The first elements of the WSU are now under development and will be available to the user community later this decade, including a wideband Band 2 receiver, a wideband upgrade to Band 6, new digitizers and digital transmission system, and soon a new correlator. Upgrades to other instruments and receiver bands are under study, including the newly developed ACA spectrometer and 2SB upgrades of Band 9 and 10 receivers for better rejection of atmospheric noise. The substantial gains in the observing efficiency enabled by the WSU will maximize the synergies between ALMA and facilities across the electromagnetic spectrum, and further enhance ALMA as the world leading facility for millimeter/submillimeter astronomy.

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An ALMA/HST Study of Millimeter Dust Emission and Star Clusters

Cited by 3 publications

References 32 publications

The dependence of the hierarchical distribution of star clusters on galactic environment

The dependence of the hierarchical distribution of star clusters on galactic environment

The Dependence of the Hierarchical Distribution of Star Clusters on Galactic Environment

The ALMA2030 Wideband Sensitivity Upgrade

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