The Age Dependence of Mid-infrared Emission around Young Star Clusters

Lin, Zhoubin; Calzetti, Daniela; Kong, Xu; Adamo, Angela; Cignoni, M.; Cook, D.; Dale, Daniel A.; Grasha, Kathryn; Grebel, Eva K.; Messa, Matteo; Sacchi, Elena; Smith, L. J.

doi:10.3847/1538-4357/ab9106

Cited by 11 publications

(55 citation statements)

References 96 publications

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“…8 Myr and 80 Myr), a visual check of the 24µm emission at the location of the cluster is used as the deciding factor. The 24 µm dust emission has been shown to follow closely the 8 µm emission in HII regions (Relaño & Kennicutt 2009), and the latter has been shown to decrease dramatically with increasing age of the star cluster out to at least 300-400 Myr (Lin et al 2020). Sharma et al (2011) showed that most of the 24 µm bright sources in M33 are generally younger than 10 Myr.…”

Section: Mamentioning

confidence: 84%

Ages and Masses of Star Clusters in M33: a Multi-wavelength Study

Moeller,

Calzetti

2021

Preprint

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We combine archival images for the nearby galaxy M33 (Triangulum Galaxy) from the ultraviolet (UV) to the infrared (IR) to derive ages, masses, and extinctions for the young star cluster population, and compare our physical parameters with published ones. Our goal is to test the robustness of clusters' ages and masses, and possibly improve on existing ones both by expanding the wavelength range of the spectral energy distribution (SED) fits and by using more recent population synthesis models. The rationale for this experiment is to verify the sensitivity of the clusters' physical parameters to observational setups and model choices that span those commonly found in the literature. We derive the physical parameters of 137 clusters, using SEDs measured in eight UV-to-I bands, including Hα, from GALEX and ground-based images. We also add the 24 µm image from the Spitzer Space Telescope to help break some age degeneracies. We find that our derived cluster ages show significant differences with earlier determinations, while the masses remain relatively insensitive to the fitting approach adopted. We also highlight an already known difficulty in recovering old, low-extinction clusters, as SED fitting codes tend to prefer younger, higher extinction solutions when the extinction is a free parameter. We publish updated ages, masses, and extinctions, with uncertainties, for all sample star clusters, together with their photometry; given the proximity of M33, this represents an important population to secure for the study of star formation and cluster evolution in spirals.

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Section: Mamentioning

confidence: 84%

Ages and Masses of Star Clusters in M33: a Multi-wavelength Study

Moeller,

Calzetti

2021

Preprint

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“…In the same Fig. 1, we compare the position of sources in our catalogs with the position of MIR compact regions, selected in Spitzer 8µm observations by Lin et al (2020). We remind that 8µm observations have a much lower resolution than the HST one, and that sources in the Lin et al (2020) catalog were selected to have some HST cluster counterpart.…”

Section: Sources With Compact Paschen-β Emissionmentioning

confidence: 99%

“…1, we compare the position of sources in our catalogs with the position of MIR compact regions, selected in Spitzer 8µm observations by Lin et al (2020). We remind that 8µm observations have a much lower resolution than the HST one, and that sources in the Lin et al (2020) catalog were selected to have some HST cluster counterpart. Overall, the different catalogs cover similar regions of the galaxy; however, some of the Lin et al (2020) sources are not present in our catalogs.…”

Section: Sources With Compact Paschen-β Emissionmentioning

confidence: 99%

“…We remind that 8µm observations have a much lower resolution than the HST one, and that sources in the Lin et al (2020) catalog were selected to have some HST cluster counterpart. Overall, the different catalogs cover similar regions of the galaxy; however, some of the Lin et al (2020) sources are not present in our catalogs. In Fig.…”

Section: Sources With Compact Paschen-β Emissionmentioning

confidence: 99%

“…Already at a few Mpc, the SF clumps observable in the MIR bands may contain several star clusters (see e.g. Lin et al 2020). Studying MIR clumps on such scales (∼ 50 pc) reveal sources with foreground extinctions up to A V ∼ 15 mag (Elmegreen & Elmegreen 2019) and are useful to study the collapse of gas clouds (Elmegreen et al 2018;Elmegreen & Elmegreen 2019, but cannot trace the effect of feedback on the ∼ pc scale.…”

Section: Introductionmentioning

confidence: 99%

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Looking for obscured young star clusters in NCG 1313

Messa,

Calzetti,

Adamo

et al. 2020

Preprint

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Using recently acquired HST NIR observations (J, Paβ and H bands) of the nearby galaxy NGC1313, we investigate the timescales required by a young star cluster to emerge from its natal cloud. We search for extincted star clusters, potentially embedded in their natal cloud as either: 1. compact sources in regions with high Hα/Paβ extinctions; 2. compact HII regions that appear as point-like sources in the Paβ emission map. The NUV-optical-NIR photometry of the candidate clusters is used to derive their ages, masses and extinctions via a least−χ 2 SED broad and narrow-band fitting process. The 100 clusters in the final samples have masses in the range log 10 (M/M ) = 2.5 − 3.5 and moderate extinctions, E(B − V)1.0 mag. Focusing on the young clusters (0 − 6 Myr) we derive a weak correlation between extinction and age of the clusters. Almost half of the clusters have low extinctions, E(B − V) < 0.25 mag, already at very young ages (≤ 3 Myr), suggesting that dust is quickly removed from clusters. A stronger correlation is found between the morphology of the nebular emission (compact, partial or absent, both in Hα and Paβ) and cluster age. Relative fractions of clusters associated with a specific nebular morphology is used to estimate the typical timescales for clearing the natal gas cloud, resulting between 3 and 5 Myr, ∼ 1 Myr older than what estimated from NUV-optical-based cluster studies. This difference hints to a bias for optically-only based studies, which JWST will address in the coming years.

show abstract

Ages and Masses of Star Clusters in M33: a Multiwavelength Study

Moeller

Calzetti

2021

View full text Add to dashboard Cite

We combine archival images for the nearby galaxy M33 (Triangulum Galaxy) from the ultraviolet (UV) to the infrared to derive ages, masses, and extinctions for the young star cluster population, and compare our physical parameters with published ones. Our goal is to test the robustness of clusters ages and masses, and possibly improve on existing ones both by expanding the wavelength range of the spectral-energy distribution (SED) fits and by using more recent population synthesis models. The rationale for this experiment is to verify the sensitivity of the clusters physical parameters to observational setups and model choices that span those commonly found in the literature. We derive the physical parameters of 137 clusters, using SEDs measured in eight UV-to-I bands, including Hα, from GALEX and ground-based images. We also add the 24 μm image from the Spitzer Space Telescope to help break some age degeneracies. We find that our derived cluster ages show significant differences with earlier determinations, while the masses remain relatively insensitive to the fitting approach adopted. We also highlight an already known difficulty in recovering old, low-extinction clusters, as SED-fitting codes tend to prefer younger, higher extinction solutions when the extinction is a free parameter. We publish updated ages, masses, and extinctions, with uncertainties for all sample star clusters, together with their photometry. Given the proximity of M33, this represents an important population to secure for the study of star formation and cluster evolution in spirals.

show abstract

The Age Dependence of Mid-infrared Emission around Young Star Clusters

Cited by 11 publications

References 96 publications

Ages and Masses of Star Clusters in M33: a Multi-wavelength Study

Ages and Masses of Star Clusters in M33: a Multi-wavelength Study

Looking for obscured young star clusters in NCG 1313

Ages and Masses of Star Clusters in M33: a Multiwavelength Study

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