A CATALOG OF EXTENDED GREEN OBJECTS IN THE GLIMPSE SURVEY: A NEW SAMPLE OF MASSIVE YOUNG STELLAR OBJECT OUTFLOW CANDIDATES

By C. Cyganowski, B. Whitney, E. Holden, Ella K. Braden, C. Brogan, E. Churchwell, R. Indebetouw, D. Watson, B. Babler, R. Benjamin and 5 more. 2008

331 citations recorded by the source corpus.

Using images from the Spitzer Galactic Legacy Infrared Mid-Plane Survey Extraordinaire (GLIMPSE), we have identified more than 300 extended 4.5 μm sources (Extended Green Objects (EGOs), for the common coding of the [4.5] band as green in three-color composite InfraRed Array Camera images). We present a catalog of these EGOs, including integrated flux density measurements at 3.6, 4.5, 5.8, 8.0, and 24 μm from GLIMPSE and the Multiband Imaging Photometer for Spitzer Galactic Plane Survey. The average angular separation between a source in our sample and the nearest IRAS point source is greater than 1′. The majority of EGOs are associated with infrared dark clouds (IRDCs), and where high-resolution 6.7 GHz CH3OH maser surveys overlap the GLIMPSE coverage, EGOs and 6.7 GHz CH3OH masers are strongly correlated. Extended 4.5 μm emission is thought to trace shocked molecular gas in protostellar outflows; the association of EGOs with IRDCs and 6.7 GHz CH3OH masers suggests that the extended 4.5 μm emission may pinpoint outflows specifically from massive protostars. The mid-IR colors of EGOs lie in regions of color–color space occupied by young protostars still embedded in infalling envelopes.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/7dafed5941055663a04eb936ee66b1d4fca7c9e9

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Citations in the corpus

INTRINSICALLY RED SOURCES OBSERVED BY SPITZER IN THE GALACTIC MIDPLANE (2008, background): “In particular, massive YSOs that appear extended at 4.5µm due to H2 and CO bandhead emission from outflows are likely to be excluded; however, a number of these are identified in the recent work by Cyganowski et al. (2008) who found over 300 such objects in the GLIMPSE I survey.”
Molecular gas kinematics within the central 250 pc of the Milky Way (2016, unknown): “44–0.102, in close proximity to an Extended Green Object (EGO; Cyganowski et al. 2008), we report a velocity dispersion of σ = 5.6kms−1 ± 0.3kms−1 (vLSR = −52.8kms−1 ± 0.3kms−1).”
CHEMISTRY IN INFRARED DARK CLOUD CLUMPS: A MOLECULAR LINE SURVEY AT 3 mm (2011, background): “A clump is called “quiescent” if it contains no IRSpitzer emission (it is IR-dark); “intermediate” if it contains either an enhanced 4.5 µm emission, the so-called “green fuzzies” (also known as Extended Green Objects (EGOs); Cyganowski et al. 2008), or a 24 µm source, but not both; “active” if it i”
FOREST Unbiased Galactic plane Imaging survey with the Nobeyama 45-m telescope (FUGIN) I: Project Overview and Initial Results (2017, background): “These surveys made a great contribution to iden- tifying star-forming activity, such as outflow from massive protostars (Cyganowski et al. 2008), new star clusters (Mercer et al. 2005), HII regions (Anderson et al. 2012), bubbles associated with star formation (Watson et al. 2008), and young…”
Characterizing precursors to stellar clusters with Herschel (2011, methodology): “Cyganowski et al. (2008) catalogued EGOs throughout the Galaxy in the GLIMPSE fields.”
A CLASS I AND CLASS II CH3OH MASER SURVEY OF EGOs FROM THE GLIMPSE SURVEY (2009, methodology): “Based on the midinfrared (MIR) colors of EGOs and their correlation with IRDCs and published 6.7 GHz CH 3 OH maser data, Cyganowski et al. (2008) argued that EGOs constitute a population of actively accreting MYSO outflow candidates.”
Hierarchical fragmentation and differential star formation in the Galactic ‘Snake’: infrared dark cloud G11.11−0.12 (2014, background): “Previous studies have shown indirect evidence of an outflow associated with P1, for example broadening of line wings, possible extended 4.5µm emission, and enrichment of outflow tracers (Carey et al. 2000; Pillai et al. 2006b; Leurini et al. 2007; Cyganowski et al. 2008; Gómez et al. 2011).”
Global collapse of molecular clouds as a formation mechanism for the most massive stars (2013, background): “The SDC335 filaments intersect at the centre of the cloud where two infrared protostars (Lbol > 2 × 104 L ; Garay et al. 2002) excite extended 4.5µm emission, a tracer of powerful outflow activity (Cyganowski et al. 2008).”
ATLASGAL — towards a complete sample of massive star forming clumps ⋆ (2014, unknown): “91−0.48 (Cyganowski et al. 2008) and AGAL327.”
STAR FORMATION IN THE CENTRAL 400 PC OF THE MILKY WAY: EVIDENCE FOR A POPULATION OF MASSIVE YOUNG STELLAR OBJECTS (2009, background): “…DR21, a massive star formation site, in which the excess 4.5µm color is considered to be due a shocked molecular outflow (Marston et al. 2004; Smith et al. 2006; Cyganowski et al. 2008) or associated with high-mass protostars within the cores of IRDCs (Rathborne et al. 2005; Beuther et al. 2005).”