Infrared Array Camera (IRAC) Colors of Young Stellar Objects

By L. Allen, N. Calvet, P. D’Alessio, B. Mer'in, L. Hartmann, S. Megeath, R. Gutermuth, J. Muzerolle, J. Pipher, P. Myers and 1 more. 2004

361 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/c564c794d96a4692f37330360f9360458096f396

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. K. Luhman
2. N. Evans II
3. P. Myers
4. L. Hartmann
5. Eric Mamajek
6. L. Hillenbrand
7. L. Allen
8. N. Calvet

In Spectroscopy

1. K. Luhman
2. N. Evans II
3. P. Myers
4. L. Hartmann
5. L. Allen
6. R. Gutermuth
7. C. Dullemond
8. J. Muzerolle

Citations in the corpus

• SDC13 infrared dark clouds: longitudinally collapsing filaments? (2013, background): “Depending on their colours, sources of different classes are expected to sit in different regions of such diagram (Allen et al. 2004; Megeath et al. 2004).”
• Spitzer Observations of NGC 1333: A Study of Structure and Evolution in a Nearby Embedded Cluster (2007, methodology): “There are now several methods in the literature to identify and classify YSOs with such photometry (cf. Allen et al. 2004; Megeath et al. 2004; Lada et al. 2006).”
• THE DISK POPULATION OF THE TAURUS STAR-FORMING REGION (2009, background): “…also appears in Luhman (2006), Luhman et al. (2006), and Kenyon et al. (2008), and probably originated in the former two papers. disks and yet they do not require knowledge of the individual stellar properties, such as spectral types and extinctions (Allen et al. 2004; Megeath et al. 2004).”
• Infrared Extinction toward Nearby Star-forming Regions (2007, methodology): “Allen et al. (2004) and Megeath et al. (2004) develop a classification scheme to differentiate young stellar objects based on their IRAC colors, and Muzerolle et al. (2004) present a scheme utilizing 24µm data in combination with IRAC data.”
• Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs (2006, background): “Many Stage I models are fairly red at [3.6]- [4.5], but are not always as red at [5.8]-[8.0] as the predictions by Allen et al. (2004).”
• The UKIDSS galactic plane survey (2007, background): “Whitney et al.2004; Churchwell et al.2004; Allen et al.2004; Megeath et al.2004).”
• The spatial distribution of star formation in the solar neighbourhood: do all stars form in dense clusters? (2010, methodology): “The Taurus and Orion YSOs are classified by using colour-colour diagrams (Allen et al. 2004; Megeath et al. 2004; Gutermuth et al. 2005, 2009).”
• A SCUBA survey of Orion -the low-mass end of the core mass function (2006, methodology): “Sources that were detected in all 4 IRAC bands were classified as Class I or Class II YSOs or as stars according to their [5.8] - [8.0] and [3.6] - [4.5] colours, as described in Allen et al. (2004).”
• The Bubbling Galactic Disk. II. The Inner 20° (2007, background): “Observations (Allen et al. 2004) and theory (Robitaille et al. 2006) predict that YSOs have steeply rising spectral energy distributions from 8 to 24 m, and hence 8Y24 m colors should be an effective discriminator of YSOs.”
• The Spitzer c2d Survey of Large, Nearby, Interstellar Clouds. IX. The Serpens YSO Population as Observed with IRAC and MIPS (2007, background): “Similarly Allen et al. (2004) have published IRAC color-color diagrams for another set of models of objects with circumstellar disks and/or envelopes.”
• Interpreting Spectral Energy Distributions from Young Stellar Objects. II. Fitting Observed SEDs Using a Large Grid of Precomputed Models (2006, methodology): “Many methods have been suggested and used in the past to classify and interpret YSO SEDs, such as spectral indices (e.g. Lada 1987) or color-color diagrams (e.g. Lada & Adams 1992; Allen et al. 2004).”
• The Disk Population of the Chamaeleon I Star-forming Region (2008, methodology): “Because of its high spatial resolution, excellent sensitivity, and large field of view, Spitzer is proficient at identifying disk-bearing members of young clusters (Allen et al. 2004; Gutermuth et al. 2004; Megeath et al. 2004; Muzerolle et al. 2004).”
• Dust Evolution and the Formation of Planetesimals (2016, methodology): “A large sample of star-forming regions/clusters with ages from 1Myr to tens of Myrs have been surveyed by various projects with Spitzer (e.g. Allen et al. 2004; Megeath et al. 2004; Luhman 2007; Evans et al. 2009; Gutermuth et al. 2009; Fang et al. 2009; Luhman et al. 2010; Megeath et al. 2012;…”
• VOSA: Virtual Observatory SED Analyzer. An application to the Collinder 69 open cluster (2008, methodology): “Barrado y Navascués et al. (2007b) studied in detail the Spitzer/IRAC data of the candidates, and based on the criteria developed by Allen et al. (2004) and Hartmann et al. (2005) derived a fraction of members with disks of 25% and 40% for the stellar and substellar population of C69, respectively.”
• THE TAURUS SPITZER SURVEY: NEW CANDIDATE TAURUS MEMBERS SELECTED USING SENSITIVE MID-INFRARED PHOTOMETRY (2009, methodology): “As our final selection mechanism, we use the IRAC color-color diagram (as seen in, e.g., Allen et al. 2004).”
• WFCAM, Spitzer/IRAC and SCUBA observations of the massive star-forming region DR21/W75 - I. The collimated molecular jets (2006, background): “In principle, IRAC colour-colour diagrams can also be used to distinguish YSO classes (Megeath et al. 2004; Allen et al. 2004; Lada et al. 2006).”
• WIDE-FIELD INFRARED SURVEY EXPLORER OBSERVATIONS OF THE EVOLUTION OF MASSIVE STAR-FORMING REGIONS (2012, background): “The basis for this scheme is the work of Allen et al. (2004) and Hartmann et al. (2005) who first investigated the distributions of young stars in Spitzer color space.”
• HIGH- AND INTERMEDIATE-MASS YOUNG STELLAR OBJECTS IN THE LARGE MAGELLANIC CLOUD (2009, background): “…YSOs are known to be surrounded by circumstellar accretion disks and envelopes, and their evolution is well established; thus, models of their spectral energy distributions (SEDs) can be generated and predictions of their locations in CMDs and CCDs can be made (e.g., Allen et al. 2004).”
• Spitzer Observations of the Orion OB1 Association: Disk Census in the Low-Mass Stars (2007, background): “The bottom right panel shows the IRAC color-color diagram, in which we identify stars with excess emission in the IRAC bands (e.g., Allen et al. 2004; Megeath et al. 2004; Hartmann et al. 2005; Sicilia-Aguilar et al. 2006; Hernández et al. 2007).”