A
                    <i>SPITZER</i>
                    SURVEY OF YOUNG STELLAR CLUSTERS WITHIN ONE KILOPARSEC OF THE SUN: CLUSTER CORE EXTRACTION AND BASIC STRUCTURAL ANALYSIS

Gutermuth, Robert; Megeath, S. T.; Myers, Philip C.; Allen, Lori; Pipher, J. L.; Fazio, G. G.

doi:10.1088/0067-0049/184/1/18

Cited by 673 publications

(1,459 citation statements)

References 73 publications

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“…The class II objects are spread out over a larger region. This result is in agreement with the IRAC study of Gutermuth et al (2009). An average extinction of A V ∼ 12 mag in the SINFONI field as derived from the extinction map seems to be consistent with the average extinction found in the previous section (Figs.…”

Section: Extinction Mapsupporting

confidence: 93%

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Sequential star formation in IRAS 06084-0611 (GGD 12-15)

Maaskant

Bik

Waters

et al. 2011

A&A

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Context. The formation and early evolution of high-and intermediate-mass stars towards the main sequence involves the interplay of stars in a clustered and highly complex environment. To obtain a full census of this interaction, the Formation and Early evolution of Massive Stars (FEMS) collaboration studies a well-selected sample of 10 high-mass star-forming regions. Aims. In this study we examine the stellar content of the high-mass star-forming region centered on IRAS 06084-0611 in the Monoceros R2 cloud. Methods. Using the near-infrared H-and K-band spectra from the VLT/SINFONI instrument on the ESO Very Large Telescope (VLT) and photometric near-infrared NTT/SOFI, 2MASS and Spitzer/IRAC data, we were able to determine the spectral types for the most luminous stars in the cluster. Results. Two very young and reddened massive stars have been detected by SINFONI: a massive young stellar object (YSO) consistent with an early-B spectral type and a Herbig Be star. Furthermore, stars of spectral type G and K are detected while still in the Pre-Main Sequence (PMS) phase. We derive additional properties such as temperatures, extinctions, radii and masses. We present a Hertzsprung-Russell diagram and find most objects having intermediate masses between ∼1.5-2.5 M . For these stars we derive a median cluster age of ∼4 Myr. Conclusions. Using Spitzer/IRAC data we confirm earlier studies that the younger class 0/I objects are centrally located while the class II objects are spread out over a larger area, with rough scale size radii of ∼0.5 pc and ∼1.25 pc respectively. Moreover, the presence of a massive YSO, an ultracompact H ii region and highly reddened objects in the center of the cluster suggest a much younger age of <1 Myr. A possible scenario for this observation would be sequential star formation along the line of sight; from a cluster of intermediate-mass to high-mass stars.

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Section: Extinction Mapsupporting

confidence: 93%

“…The data were downloaded from the archive and processed using the MOPEX software version 16.2.1 (Makovoz et al 2006). Spitzer/IRAC photometry of IRAS 06084-0611 has previously been studied in Gutermuth et al (2009).…”

Section: Photometry: Spitzer/irac 2mass and Ntt/sofi Observationsmentioning

confidence: 99%

Sequential star formation in IRAS 06084-0611 (GGD 12-15)

Maaskant

Bik

Waters

et al. 2011

A&A

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“…Once this is done for the YSOs we separate the Class I/II objects. Σ is calculated this way since Class Is and Class IIs are not always spatially distinct from one another [21]. Class IIs are known to be slightly more dispersed than Class Is in high density regions [21] reflecting early dynamical evolution.…”

Section: Resultsmentioning

confidence: 99%

“…Σ is calculated this way since Class Is and Class IIs are not always spatially distinct from one another [21]. Class IIs are known to be slightly more dispersed than Class Is in high density regions [21] reflecting early dynamical evolution. However, the similar distribution between these classes leads us to conclude that the distribution of observed Σ is mainly primordial in nature.…”

Section: Resultsmentioning

confidence: 99%

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Do All Stars in the Solar Neighbourhood Form in Clusters?

Bressert

Bastian

Gutermuth

2011

Star Clusters in the Era of Large Surveys

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We present a global study of low mass, young stellar object (YSO) surface densities (Σ ) in nearby (< 500 pc) star forming regions based on a comprehensive collection of Spitzer Space Telescope surveys. We show that the distribution of YSO surface densities is a smooth distribution, being adequately described by a lognormal function from a few to 10 3 YSOs per pc 2 , with a peak at ∼ 22 stars pc −2 . The observed lognormal Σ is consistent with predictions of hierarchically structured starformation at scales below 10 pc, arising from the molecular cloud structures. We do not find evidence for multiple discrete modes of star-formation (e.g. clustered and distributed). Comparing the observed Σ distribution to previous Σ threshold definitions of clusters show that they are arbitrary. We find that only a low fraction (< 26%) of stars are formed in dense environments where their formation/evolution (along with their circumstellar disks and/or planets) may be affected by the close proximity of their low-mass neighbours.

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Star Formation at High Resolution, Zooming into the Carina Nebula, the Nearest Laboratory of Massive Star Feedback

Preibisch

2011

Reviews in Modern Astronomy

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A SPITZER SURVEY OF YOUNG STELLAR CLUSTERS WITHIN ONE KILOPARSEC OF THE SUN: CLUSTER CORE EXTRACTION AND BASIC STRUCTURAL ANALYSIS

Cited by 673 publications

References 73 publications

Sequential star formation in IRAS 06084-0611 (GGD 12-15)

Sequential star formation in IRAS 06084-0611 (GGD 12-15)

Do All Stars in the Solar Neighbourhood Form in Clusters?

Star Formation at High Resolution, Zooming into the Carina Nebula, the Nearest Laboratory of Massive Star Feedback

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