Difference between revisions of "ProtostarsInNGC281"
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===Introduction to NGC 281=== | ===Introduction to NGC 281=== | ||
NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (<math>\alpha</math>2000=00h52m, <math>\delta</math>2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. <br/><br/> | NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (<math>\alpha</math>2000=00h52m, <math>\delta</math>2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia. <br/><br/> | ||
| − | ''' | + | '''NGC 281 contains several distinct regions:''' |
| − | NGC 281 contains several distinct regions:''' | + | *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.<br/> |
| − | *an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005 | + | *Two quite distinct CO molecular clouds: |
| − | *Two quite distinct CO molecular clouds | + | **The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system. |
| − | **The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 | + | **NGC 281 West (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath & Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders. |
| − | |||
| − | **NGC 281 West (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath & Wilson 1997). The region is heavily obscured by dust | ||
Revision as of 13:33, 6 December 2013
The idea is to start gathering two items:
- Relevant figures
- Text and references.
Contents
Abstract
- Carol.
Introduction to NGC 281
NGC 281 is an active star-forming nebulosity about 2.81± 0.24 kpc or 9200 light-years away (Sato et al. 2008) at a relatively high galactic latitude (Failed to parse (MathML with SVG or PNG fallback (recommended for modern browsers and accessibility tools): Invalid response ("Math extension cannot connect to Restbase.") from server "https://en.wikipedia.org/api/rest_v1/":): {\displaystyle \alpha}
2000=00h52m, Failed to parse (MathML with SVG or PNG fallback (recommended for modern browsers and accessibility tools): Invalid response ("Math extension cannot connect to Restbase.") from server "https://en.wikipedia.org/api/rest_v1/":): {\displaystyle \delta}
2000=+56d34m or l=123.1deg, b= -6.3deg) in the constellation Cassiopeia.
NGC 281 contains several distinct regions:
- an HII emission region Sharpless 184 of diameter 20 arcminutes containing the young galactic cluster IC 1590 centered about the OB star trapezium system HD5005.
- Two quite distinct CO molecular clouds:
- The southeastern CO region (N281A) with local standard of rest (LSR) similar to that of the HII region itself (-30.5 km/s vs. -26.5 km/s). This region contains highly recognizable “pillars of creation.” These pillars are known to contain newborn stars as a result of triggering from the nearby OB star trapezium system.
- NGC 281 West (N281B), a molecular cloud in the southwestern region with three distinct clumps (NE, NW and S) (Megeath & Wilson 1997). The region is heavily obscured by dust and has a LSR (+44 km/s) quite different from that of its eastern neighbor and the HII region it borders.
Protostar basics
- Lynn
Two Scenarios for Star Formation
- Peggy
Spontaneous vs. Triggered Star Formation
• Most star formation begins due to spontaneous processes on a galactic scale, given sufficient time and material free fall will result in star formation.
• An outside source of energy can trigger the formation of a star before conditions become sufficient for free fall, leaving sequentially younger stars in its path while clouds broken into filaments by magnetic fields will show a filamentary pattern of protostars.
Star formation in a “controlled” environment
• small regions where the formation conditions except for the trigger are the same
• physical and geographical characteristics of protostars created can therefore be related to triggering mechanism.
NGC 281
• HII emission containing the young galactic cluster IC 1590, OB star trapezium system HD5005 with what appears to be two distinct start forming regions around it;
• Triggered East side with “pillars of creation”, newborn stars as a result of triggering from the nearby OB star trapezium system.
• Crowded West side with three distinct clumps (NE, NW and S) of star formation.
Herschel data
- Carol
Spitzer data
- Melissa
Source Identification
- Carol
Photometry Using APT
- Lynn
Final Source Selection
- Melissa
- Peggy
Analysis & Results
- TBD
Discussion & Conclusions
- TBD
List of References
- TBD
List of Authors & Affiliations
- Carol
