Please use this identifier to cite or link to this item:
|Title:||KFPA Examinations of Young STellar Object Natal Environments (KEYSTONE): Hierarchical Ammonia Structures in Galactic Giant Molecular Clouds||Authors:||Keown, Jared
Di Francesco, James
Anderson, L. D.
Chen, Michael Chun-Yuan
ELIA, Davide Quintino
Myers, Philip C.
Offner, Stella S. R.
|Issue Date:||2019||Journal:||THE ASTROPHYSICAL JOURNAL||Number:||884||Issue:||1||Abstract:||We present initial results from the K-band Focal Plane Array Examinations of Young STellar Object Natal Environments survey, a large project on the 100 m Green Bank Telescope mapping ammonia emission across 11 giant molecular clouds at distances of 0.9-3.0 kpc (Cygnus X North, Cygnus X South, M16, M17, Mon R1, Mon R2, NGC 2264, NGC 7538, Rosette, W3, and W48). This data release includes the NH<SUB>3</SUB> (1,1) and (2,2) maps for each cloud, which are modeled to produce maps of kinetic temperature, centroid velocity, velocity dispersion, and ammonia column density. Median cloud kinetic temperatures range from 11.4 ± 2.2 K in the coldest cloud (Mon R1) to 23.0 ± 6.5 K in the warmest cloud (M17). Using dendrograms on the NH<SUB>3</SUB> (1,1) integrated intensity maps, we identify 856 dense gas clumps across the 11 clouds. Depending on the cloud observed, 40%-100% of the clumps are aligned spatially with filaments identified in H<SUB>2</SUB> column density maps derived from spectral energy distribution fitting of dust continuum emission. A virial analysis reveals that 523 of the 835 clumps (∼63%) with mass estimates are bound by gravity alone. We find no significant difference between the virial parameter distributions for clumps aligned with the dust-continuum filaments and those unaligned with filaments. In some clouds, however, hubs or ridges of dense gas with unusually high mass and low virial parameters are located within a single filament or at the intersection of multiple filaments. These hubs and ridges tend to host water maser emission, multiple 70 μm detected protostars, and have masses and radii above an empirical threshold for forming massive stars.||URI:||http://hdl.handle.net/20.500.12386/29132||URL:||https://iopscience.iop.org/article/10.3847/1538-4357/ab3e76||ISSN:||0004-637X||DOI:||10.3847/1538-4357/ab3e76||Bibcode ADS:||2019ApJ...884....4K||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
Show full item record
Files in This Item:
|_Keown_et_al._ApJ.pdf||Pdf editoriale||21.52 MB||Adobe PDF||View/Open|
|29132-_Keown_et_al._ApJ_P01.pdf||Miur||9.34 MB||Adobe PDF|
|29132-_Keown_et_al._ApJ_P02.pdf||Miur||9.26 MB||Adobe PDF|
|29132-_Keown_et_al._ApJ_P03.pdf||Miur||3.01 MB||Adobe PDF|
checked on Jul 25, 2021
checked on Jul 25, 2021
Items in DSpace are published in Open Access, unless otherwise indicated.