MIPSGAL: A Survey of the Inner Galactic Plane at 24 and 70 μm

Carey, Sean; Noriega-Crespo, A.; Mizuno, D. R.; Shenoy, S.; Paladini, R.; Kraemer, K. E.; Price, S. D.; Flagey, Nicolas; Ryan, Erin L.; Ingalls, James G.; Kuchar, T. A.; Gonçalves, D. Pinheiro; Indebetouw, R.; Billot, N.; Marleau, F.; Padgett, Deborah; Rebull, L. M.; Bressert, E.; Ali, B.; Molinari, S.; Martín, P. G.; Berriman, G. Bruce; Boulanger, F.; Latter, William B.; Miville-Deschênes, M.-A.; Shipman, R.; Testi, L.

doi:10.1086/596581

Cited by 591 publications

(148 citation statements)

References 75 publications

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“…5 The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under agreement by Associated Universities, Inc. Overview of the NGC 6334 I(N) region in the mid-infrared. The three-color image was generated from the Spitzer MIPSGAL and GLIMPSE survey images at 24, 4.5, and 3.6 μm (Benjamin et al 2003;Churchwell et al 2009;Carey et al 2009). For reference the SMA compact + extended (COMP+EXT) configuration 1.3 mm continuum with 2.…”

Section: Observationsmentioning

confidence: 99%

Subarcsecond Imaging of the NGC 6334 I(n) Protocluster: Two Dozen Compact Sources and a Massive Disk Candidate

Hunter

Brogan

Cyganowski

et al. 2014

ApJ

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Using the Submillimeter Array (SMA) and Karl G. Jansky Very Large Array, we have imaged the massive protocluster NGC 6334 I(N) at high angular resolution (0. 5 ∼ 650 AU) from 6 cm to 0.87 mm, detecting 18 new compact continuum sources. Three of the new sources are coincident with previously identified H 2 O masers. Together with the previously known sources, these data bring the number of likely protocluster members to 25 for a protostellar density of ∼700 pc −3 . Our preliminary measurement of the Q-parameter of the minimum spanning tree is 0.82-close to the value for a uniform volume distribution. All of the (nine) sources with detections at multiple frequencies have spectral energy distributions consistent with dust emission, and two (SMA 1b and SMA 4) also have long wavelength emission consistent with a central hypercompact H ii region. Thermal spectral line emission, including CH 3 CN, is detected in six sources: LTE model fitting of CH 3 CN (J = 12-11) yields temperatures of 72-373 K, confirming the presence of multiple hot cores. The fitted LSR velocities range from −3.3 to −7.0 km s −1 , with an unbiased mean square deviation of 2.05 km s −1 , implying a protocluster dynamical mass of 410 ± 260 M . From analysis of a wide range of hot core molecules, the kinematics of SMA 1b are consistent with a rotating, infalling Keplerian disk of diameter 800 AU and enclosed mass of 10-30 M that is perpendicular (within 1• ) to the large-scale bipolar outflow axis. A companion to SMA 1b at a projected separation of 0. 45 (590 AU; SMA 1d), which shows no evidence of spectral line emission, is also confirmed. Finally, we detect one 218.4400 GHz and several 229.7588 GHz Class-I CH 3 OH masers.

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Section: Observationsmentioning

confidence: 99%

Subarcsecond Imaging of the NGC 6334 I(n) Protocluster: Two Dozen Compact Sources and a Massive Disk Candidate

Hunter

Brogan

Cyganowski

et al. 2014

ApJ

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“…• > l > −65 • for |b| < 1 • , at 24 and 70 μm (Carey et al 2009) which avoided duplicating coverage of the Galactic center region. MIPSGAL-II post-BCD data were used to fill gaps around the high latitude edges.…”

Section: Mips Survey At 24 μMmentioning

confidence: 99%

Star Formation in the Central 400 Pc of the Milky Way: Evidence for a Population of Massive Young Stellar Objects

Yusef‐Zadeh

Hewitt

Arendt

et al. 2009

ApJ

204

264

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The central kpc of the Milky Way might be expected to differ significantly from the rest of the Galaxy with regard to gasdynamics and the formation of young stellar objects (YSOs). We probe this possibility with midinfrared observations obtained with Infrared Array Camera and Multiband Imaging Photometer on Spitzer and with Midcourse Space Experiment. We use color-color diagrams and spectral energy distribution (SED) fits to explore the nature of YSO candidates (including objects with 4.5 μm excesses possibly due to molecular emission). There is an asymmetry in the distribution of the candidate YSOs, which tend to be found at negative Galactic longitudes; this behavior contrasts with that of the molecular gas, approximately 2/3 of which is at positive longitudes. The small-scale height of these objects suggests that they are within the Galactic center region and are dynamically young. They lie between two layers of infrared dark clouds and may have originated from these clouds. We identify new sites for this recent star formation by comparing the mid-IR, radio, submillimeter, and methanol maser data. The methanol masers appear to be associated with young, embedded YSOs characterized by 4.5 μm excesses. We use the SEDs of these sources to estimate their physical characteristics; their masses appear to range from ∼10 to ∼20 M . Within the central 400 × 50 pc (|l| < 1.• 3 and |b| < 10 ) the star formation rate (SFR) based on the identification of Stage I evolutionary phase of YSO candidates is about 0.14 M yr −1 . Given that the majority of the sources in the population of YSOs are classified as Stage I objects, we suggest that a recent burst of star formation took place within the last 10 5 yr. This suggestion is also consistent with estimates of SFRs within the last ∼10 7 yr showing a peak around 10 5 yr ago. Lastly, we find that the Schmidt-Kennicutt Law applies well in the central 400 pc of the Galaxy. This implies that star formation does not appear to be dramatically affected by the extreme physical conditions in the Galactic center region.

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“…It includes the standard "read-2," row-droop, and droop corrections, dark subtraction, flat fielding, and a modified linearization. The optimization involves better artifact mitigation such as overlap, jailbar, and latent corrections; additional details are described by Mizuno et al (2008) and Carey et al (2009). The 70 μm data are not considered here and thus are not described.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Circumstellar Structure Around Evolved Stars in the Cygnus-X Star Formation Region

Kraemer¹,

Hora

Egan

et al. 2010

The Astronomical Journal

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We present observations of newly discovered 24 μm circumstellar structures detected with MIPS around three evolved stars in the Cygnus-X star-forming region. One of the objects, BD+43 3710, has a bipolar nebula, possibly due to an outflow or a torus of material. A second, HBHA 4202-22, a Wolf-Rayet candidate, shows a circular shell of 24 μm emission suggestive of either a limb-brightened shell or disk seen face-on. No diffuse emission was detected around either of these two objects in the Spitzer 3.6-8 μm IRAC bands. The third object is the luminous blue variable candidate G79.29+0.46. We resolved the previously known inner ring in all four IRAC bands. The 24 μm emission from the inner ring extends ∼1. 2 beyond the shorter wavelength emission, well beyond what can be attributed to the difference in resolutions between MIPS and IRAC. Additionally, we have discovered an outer ring of 24 μm emission, possibly due to an earlier episode of mass loss. For the two shell stars, we present the results of radiative transfer models, constraining the stellar and dust shell parameters. The shells are composed of amorphous carbon grains, plus polycyclic aromatic hydrocarbons in the case of G79.29+0.46. Both G79.29+0.46 and HBHA 4202-22 lie behind the main Cygnus-X cloud. Although G79.29+0.46 simply may be on the far side of the cloud, HBHA 4202-22 is unrelated to the Cygnus-X star formation region.

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MIPSGAL: A Survey of the Inner Galactic Plane at 24 and 70 μm

Cited by 591 publications

References 75 publications

Subarcsecond Imaging of the NGC 6334 I(n) Protocluster: Two Dozen Compact Sources and a Massive Disk Candidate

Subarcsecond Imaging of the NGC 6334 I(n) Protocluster: Two Dozen Compact Sources and a Massive Disk Candidate

Star Formation in the Central 400 Pc of the Milky Way: Evidence for a Population of Massive Young Stellar Objects

Circumstellar Structure Around Evolved Stars in the Cygnus-X Star Formation Region

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