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Embedded Star Formation and Circumstellar Disk Evolution: Early Results from MIPS

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Embedded Star Formation and Circumstellar Disk Evolution: Early Results from MIPS The Spitzer Space Telescope: New Views of the Cosmos ASP Conference Series, Vol. 357, 2006 L. Armus and W.T. Reach Embedded Star Formation and Circumstellar Disk Evolution: Early Results from MIPS Erick T. Young and James Muzerolle Steward Observatory, 933 N Cherry Ave, Tucson AZ 85721 Abstract. We present some recent results from the Guaranteed Time Young Clusters program, with particular emphasis on results from the MIPS instru- ment. In this program we have surveyed some of the best examples of nearby clusters using both IRAC and MIPS. The clusters range in age from less than 1 Myr to over 100 Myr, and they represent a variety of environments with regard to the presence of massive stars. In the youngest clusters, the MIPS observations show star formation occuring on large scales in coherent structures that trace out the dense gas. In the older clusters in our sample, the circumstellar material has disappeared around most of the stars, but a small fraction of the sources show evidence for debris disks. 1. Introduction The Spitzer Space Telescope represents a significant advancement in our capabil- ities to study star formation in young clusters. First, the sensitivity of the cryo- genic facility now means that even the lowest mass protostars are within reach. Second, the advent of large format infrared detectors means that large areas can be efficiently mapped, particularly in the far infrared. Specifically, the Scan-map mode of the MIPS instrument allows coverage of degree scale areas with min- imal overhead associated with the repositioning of the telescope. Spitzer also provides unprecedented photometric stability at the long wavelengths, enabling studies of even modest infrared excesses around stars. Finally and surprisingly, the angular resolution of the 85 cm telescope is a key attribute in star formation studies. Despite being seriously diffraction limited at the longer wavelengths, Spitzer still provides much better angular detail than previous missions. Circumstellar disks are a key element in the formation of all stars, providing the mechanism that transfers material from the parent cloud onto the forming star. It is now widely accepted that the timescale for this main accretion phase is quite short, only a few million years (e.g., Robberto et al. 1999; Lada et al. 2000; Haisch et al. 2001). The details of the dispersal of the accretion disk, however, are not well known. Since most previous studies have been conduced at near- infrared wavelengths, only the inner parts of these disks have been investigated, and many questions remain unsettled. Do disks clear out by initially forming an inner hole? How complete is the disk dispersal many AU from the star? What is the effect of the environment? Are dispersal timescales dependent of the mass of the star? How early are debris disks formed? We report on some initial results from a MIPS guaranteed time program to study the evolution of disks in young clusters. In this program, we have mapped clusters ranging in age from less than 1 Myr to over 100 Myr. The ability of 101 102 Young and Muzerolle Spitzer to efficiently map large regions at great sensitivity provides a unique ability to investigate disk evolution for many stars. 2. Observing Program Clusters are excellent laboratories for studying disk evolution. By mapping clusters, data for hundreds of roughly coeval stars can be efficiently collected. Although some uncertainty still exists on the absolute calibration of cluster ages, the relative ages of the clusters in the sample is fairly unambiguous. For this program, we have selected some of the best studied examples of nearby young clusters. Typically, the regions are less than 1 kpc distance, which means that we will be able to detect the photospheres of even substellar ojects with IRAC. For the nearest clusters, the MIPS 24 µm band can detect the photo- spheres of solar-type stars. Because the regions tend to occupy large regions on the sky, efficiency of the MIPS Scan Map mode (Rieke et al. 2004) is used to advdantage. To provide full spectral coverage, we have also done IRAC mapping of the same clusters. The IRAC mapping has been done in collaboration with members of the IRAC instrument team. Table 1 presents the regions in our program. Table 1. MIPS Young Cluster Program Region Age Distance Map Size (Myr) (pc) (arcmin) ρ Oph <1 150 4 x 60 x 60 NGC 1333 <1 320 30 x 30 Trapezium ∼1 450 60 x 60 NGC 2068 & 2071 1 - 3 415 45 x 35 σ Ori 2 350 45 x 35 IC 348 3 320 30 x 30 NGC 2244 3 - 5 1600 30 x 30 NGC 2264 5 800 45 x 35 NGC 7160 5 600 30 x 30 NGC 869 12 2240 30 x 30 NGC 884 12 2240 30 x 30 IC 2395 16 850 45 x 35 NGC 2547 25 450 45 x 35 NGC 2451 40 190 45 x 35 IC 2391 55 150 45 x 35 Pleiades 130 150 60 x 30, 45 x 35 NGC 2516 160 350 30 x 30 2.1. NGC 2547 The first cluster observed under this program (Young et al. 2004) was NGC 2547, a 25 Myr old cluster in Vela. Of the several thousand sources detected in our observations, we selected a subset of 162 stars that were probable cluster members based on previous ground-based photometry and spectroscopy. Not Embedded Star Formation and Disk Evolution 103 surprisingly, we found no evidence of infrared excess at 3.6 or 4.5 µm for most of the stars. For the lowest mass stars (spectral type later than ∼K5), however, a snall fraction appears to have excesses. In Figure 1, we show the J - K , K - [3.6 µm] and J - K , K - [4.5 µm] color-color diagram overlaid with the intrinsic colors of stars from Patten et al. (2005). Deeper observations, particularly at longer wavelengths will test the validity of this result. 2.0 2.0 1.5 1.5 ) ) s s 1.0 1.0 e e ud ud it it 0.5 0.5 agn agn M M ( ( K K - 0.0 - 0.0 J J -0.5 -0.5 -1.0 -1.0 -1.0 -0.5 0.0 0.5 1.0 1.5 2.0 -1.0 -0.5 0.0 0.5 1.0 1.5 2.0 P K - [3.6 P m] (Magnitudes) K - [4.5 m] (Magnitudes) Figure 1. (a) J - K, K - 3.6 µm color-color diagram for the 162 candidate members of the cluster. The intrinsic colors for dwarfs are plotted as solid lines. (B) J - K, K - 4.5 µm color-color diagram. 2.2. NGC 2068/2071 At a distance of 415 pc, the Orion B complex is the closest giant molecular cloud. Included in the region are the prominent star forming regions NGC 2023, 2024, 2068 and 2071. The well studied NGC 2068/2071 region has been mapped in numerous molecular tracers as well as 850 µm continuum (Mitchell et al. 2001). With a wealth of sub-millimeter sources, HH-objects, and dense gas, NGC 2068/2071 is clearly a site of ongoing, active star formation. As part of this program, the cloud has been mapped by Spitzer with both IRAC and MIPS. Most striking is the Spitzer 24 µm image. This wavelength is particularly useful in the study of very young regions since it is long enough in wavelength and sensitive enough to detect the embedded Class I and even Class 0 objects. It is short enough in wavelength, however, to have good angular resolution with Spitzer. We show part the 24 µm NGC 2068 image in Figure 2 along side the corresponding 70 µm map. The remarkable lining up of the Spitzer sources along the edge of the cloud drives one to the conclusion that the star formation is externally triggered, perhaps by the interaction of the dense molecular cloud with the nearby HII region. 3. Summary In this program, we have observed regions of ages <1 Myr to 160 Myr. In the 25 Myr old cluster NGC 2547, we have found that the disks are well cleared. The few excess candidates are all low mass members of the cluster. In the very 104 Young and Muzerolle Figure 2. (a) Spitzer 24 µm image of NGC 2068. (b) Corresponding 70 µm frame. young cluster NGC 2068, the prominent far-infrared (and presumably youngest) sources are all located along a line defined by the dense edge of the cloud, suggesting a triggering mechanism for the star formation. Acknowledgments. This work is based on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California Institute of Technology under NASA contract 1407. Support for this work was provided by NASA through Contract Number 960785 issued by JPL/Caltech. References Haisch, K.E., Jr., Lada, E.A., & Lada, C.J. 2001, ApJ, 553, L153. Lada, C. J., Muench, A., Haisch, K. E., Lada, E. A., Alver, J. F., Tollestrup, E. V., & Willner, S. 2000, AJ, 120, 3162. Mitchell,G.F., Johnstone, D., Moriarty-Schieven, G., Fich, M., & Tothill, N.F.H. 2001, ApJ,556, 215. Patten, B. M., Henry, T. J., Burrows, A., Stauffer, J. R., Raghavan, D., Liebert, J., Luhman, K. L., Hora, J. L., Megeath, S. T., Marengo, M., & Fazio, G. G.,2005,BAAS,205,11.10. Rieke, G.H., et al. 2004,ApJS, 154, 25. Robberto, M., Meyer, M. R., Natta, A., & Beckwith, S. V. W. 1999, The Universe as Seen by ISO. Eds. P. Cox & M. F. Kessler. ESA-SP 427., p. 195.
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