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| Serpens Main | |
|---|---|
| Name | Serpens Main |
| Type | Star-forming region |
| Constellation | Serpens |
| Distance | ~415 pc |
| Epoch | J2000 |
| Notable objects | Serpens South, Serpens Cluster A, SVS 4, SMM1 |
Serpens Main is a nearby star-forming region within the Serpens constellation notable for dense molecular gas, protostellar clusters, and rich infrared and millimeter emission. The region has been studied by observatories such as Spitzer Space Telescope, Herschel Space Observatory, Atacama Large Millimeter/submillimeter Array, and James Clerk Maxwell Telescope, and appears in catalogs from Two Micron All Sky Survey, WISE, and ground-based surveys. Astronomers connect studies of this region to broader research on Orion Nebula, Taurus Molecular Cloud, Perseus molecular cloud, and Aquila Rift star formation environments.
Serpens Main is a compact, active star-forming complex characterized by clustered young stellar objects, dense cores, and filamentary structure; it is often compared to regions such as Ophiuchus molecular cloud, Rho Ophiuchi, NGC 1333, and IC 348. Observations by instruments including Very Large Array, Submillimeter Array, IRAM 30m telescope, and Green Bank Telescope have mapped its protostellar population, revealing Class 0 and Class I objects similar to those in L1688, L1495, and Bok globules. Studies published by teams at institutions such as Harvard–Smithsonian Center for Astrophysics, Max Planck Institute for Astronomy, California Institute of Technology, and National Radio Astronomy Observatory place Serpens Main among well-studied nearby sites alongside Cepheus Flare and Chamaeleon I.
Located in the northern part of the constellation Serpens, the complex lies near the Galactic plane and is often associated in distance estimates with structures seen toward Aquila Rift and Scutum–Centaurus Arm. Its projected coordinates place it adjacent to regions cataloged by surveys like Barnard Catalogue and LDN (Lynds) catalog. The structure contains dense clumps identified in CO isotopologue maps from James Clerk Maxwell Telescope and Nobeyama Radio Observatory, and continuum peaks mapped by Bolocam and SCUBA-2. Filamentary morphology resembles features in Herschel Gould Belt Survey fields such as in Vela C and Polaris Flare.
The region hosts a population of embedded protostars, young stellar objects, and pre-main-sequence stars comparable to those cataloged in Spitzer Space Telescope studies of Cepheus and Lupus. Protostellar outflows traced in CO and SiO by ALMA and SMA show jets and molecular bullets similar to phenomena in HH 211, L1448, and Orion KL. Infrared excess sources identified by 2MASS, Spitzer, and WISE photometry reveal disks analogous to those around stars in T Tauri stars populations and Herbig Ae/Be stars clusters studied at Keck Observatory and Very Large Telescope. Age estimates and initial mass function analyses have been undertaken by research groups at University of California, Berkeley, University of Michigan, and Princeton University.
Molecular line surveys of CO, 13CO, C18O, N2H+, NH3, and HCO+ from facilities such as IRAM, GBT, and Nobeyama Radio Observatory characterize the cloud’s temperature, turbulence, and column density. Observed kinetic temperatures and velocity dispersions are compared with measurements in Perseus, Orion A, and Pipe Nebula to assess fragmentation. Studies by teams from University of Arizona and Leiden Observatory used radiative transfer modeling and chemical networks similar to those applied to Barnard 1 and IC 348 to infer depletion and deuteration levels. Magnetic field measurements via polarized dust emission and Zeeman splitting using Planck (spacecraft) and Arecibo Observatory provide constraints analogous to those for Taurus and Ophiuchus.
Key subregions and objects within the complex have been identified in continuum and line surveys, including dense cores and infrared clusters that parallel features named in other clouds such as NGC 1333 and Serpens South. Prominent sources studied with interferometers include protostars with catalog names from IRAS, SMM designations, and submillimeter peaks cataloged in Bolocam Galactic Plane Survey. Outflow-driving sources are compared to classical objects like HH 212 and HH 34. Embedded clusters have been analyzed in the context of cluster formation studies at Carnegie Institution for Science and Smithsonian Astrophysical Observatory.
Serpens Main has been targeted by large surveys including the Herschel Gould Belt Survey, Spitzer c2d (From Cores to Disks), and ground-based millimeter continuum surveys such as JCMT Gould Belt Survey. Radio through infrared campaigns have utilized ALMA, VLA, SMA, IRAM 30m telescope, and space telescopes like Spitzer Space Telescope and Herschel Space Observatory. Data products appear in archives maintained by NASA/IPAC, European Space Agency, and observatory data centers at NRAO and ALMA Science Archive. Comparative analyses reference methodologies from surveys of Taurus Molecular Cloud and Aquila Rift.
The region forms part of the larger Serpens Cloud Complex, which includes neighboring concentrations such as Serpens South and other clouds studied in surveys of the Gould Belt and Aquila Rift. Its membership and distance relationships have been debated in the literature alongside determinations for Serpens South Cluster and estimates using Gaia parallaxes, similar to distance revisions made for Orion Nebula Cluster and Taurus. Studies by research groups at University of Vienna, ETH Zurich, and MPIA integrate Serpens Main into multi-cloud models of star formation used to compare environments like Lupus and Chamaeleon.
Category:Star-forming regions