Αποτελέσματα - Λεπτομέρειες
Εντολή Αναζήτησης : Συγγραφέας="Ζέζας"
Και Συγγραφέας="Ανδρέας"
Τρέχουσα Εγγραφή: 7 από 44
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| Τίτλος |
Star-cluster populations and X-ray binaries in NGC 2276 |
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Συγγραφέας
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Κωτούλας, Παναγιώτης
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Σύμβουλος διατριβής
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Ζέζας, Ανδρέας
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| Περίληψη |
The age and mass of star-cluster populations within a galaxy can be used to trace its star formation history. The spiral galaxy NGC2276, member of the NGC2300 galaxy group, provides an interesting laboratory to study the effects of galaxy harassment on star-formation and cluster populations. The galaxy’s west side is compressed due to its super-sonic movement within the intra-group medium, possibly triggering star formation (Rasmussen et al., 2006; Wolter et al., 2015). This asymmetry is evident both in optical and X-ray images, with the west side having an X-ray luminosity ∼ 5 times greater than the east side (Anastasopoulou et al., 2019).We use Hubble Space Telescope WFC3-UVIS observations of the galaxy in order to detect the clusters and perform photometry. We estimate the cluster ages by comparing our data to evolutionary tracks obtained by using two different stellar population synthesis models; one utilizing the MIST and the other the BPASS isochrones. We estimate that most of the clusters have ages ∼ 10 − 100 Myrs, while the BPASS model seems to be in better agreement with our data. Using spectral energy distribution fits we are able to derive the age, mass and extinction for a selection of clusters. Ages fall within the 10 − 100 Myr range, while masses fall in the 103 − 103 M⊙ range. The MIST model indicates that the east region clusters might experience smaller extinction in contrast to clusters located in other regions. Cluster masses and ages are consistent between different regions. Finally, we match the X-ray sources catalogue of Anastasopoulou et al., 2019 to our clusters catalogue and perform a spectral energy distribution fit for the best matches. In most cases, clusters in the vicinity of X-ray sources have young ages (< 100 Myr) and large masses, indicating that the corresponding X-ray source is likely a High-Mass X-ray Binary.
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| Γλώσσα |
Αγγλικά |
| Ημερομηνία έκδοσης |
2023-07-28 |
| Συλλογή
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Σχολή/Τμήμα--Σχολή Θετικών και Τεχνολογικών Επιστημών--Τμήμα Φυσικής--Πτυχιακές εργασίες
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Τύπος Εργασίας--Πτυχιακές εργασίες
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| Μόνιμη Σύνδεση |
https://elocus.lib.uoc.gr//dlib/c/8/8/metadata-dlib-1689667062-571108-17951.tkl
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| Εμφανίσεις |
172 |
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