THE HUBBLE SPACE TELESCOPE TREASURY PROGRAM ON THE ORION NEBULA CLUSTER ^,

Abstract

The Hubble Space Telescope (HST) Treasury Program on the Orion Nebula Cluster has used 104 orbits of HST time to image the Great Orion Nebula region with the Advanced Camera for Surveys (ACS), the Wide-Field/Planetary Camera 2 (WFPC2) and the Near Infrared Camera and Multi Object Spectrograph (NICMOS) instruments in 11 filters ranging from the U-band to the H-band equivalent of HST. The program has been intended to perform the definitive study of the stellar component of the ONC at visible wavelengths, addressing key questions like the cluster IMF, age spread, mass accretion, binarity and cirumstellar disk evolution. The scanning pattern allowed to cover a contiguous field of approximately 600 square arcminutes with both ACS and WFPC2, with a typical exposure time of approximately 11 minutes per ACS filter, corresponding to a point source depth AB(F435W) = 25.8 and AB(F775W)=25.2 with 0.2 magnitudes of photometric error. We describe the observations, data reduction and data products, including images, source catalogs and tools for quick look preview. In particular, we provide ACS photometry for 3399 stars, most of them detected at multiple epochs, WFPC2 photometry for 1643 stars, 1021 of them detected in the U-band, and NICMOS JH photometry for 2116 stars. We summarize the early science results that have been presented in a number of papers. The final set of images and the photometric catalogs are publicly available through the archive as High Level Science Products at the STScI Multimission Archive hosted by the Space Telescope Science Institute.

A MUSE map of the central Orion Nebula (M 42)

“…We therefore have to assume that the zeropoints applied by Da Rio et al include an unknown component that causes a shift of the central effective wavelength of the red filters, but less of a shift for the green filter 8 . Since the Orion Nebula is too bright for SDSS stellar photometry to work and all four stars are marked as saturated in the HST ACS catalog of Robberto et al (2013), we cannot cross-check our reconstructed magnitudes with a betterstudied photometric system.…”

A Candidate Planetary-Mass Object With a Photoevaporating Disk in Orion

“…(J2000.0) = −05°23′52 99 is located southwest of θ 1 Ori C. The projected distance between them is about 0.11 pc. In Figure 1, we show the HST ACS color-composite image of Proplyd 133-353 using the HST images from Robberto et al (2013). The tail can be clearly seen in the HST image in the F658N band (green emission) and extends out to 190 au.…”

“…The tail can be clearly seen in the HST image in the F658N band (green emission) and extends out to 190 au. We visually inspected the HST images of the object in different bands from Robberto et al (2013) and found that the tail can also be clearly detected in the F435W band for ACS/WFC, and the F336W and F656N bands for WFPC2, which could be due to the tail showing strong Balmer emission lines, e.g., Hα (F658N), Hγ (F435W), and Balmer continuum emission (F336W).…”

Herschel-Planckdust optical-depth and column-density maps

“…Maddalena et al 1986;Blaauw 1991;Brown et al 1995;Wilson et al 2005;Bally 2008;Lombardi et al 2011), is probably the most often studied molecular-cloud complex (see Bally 2008;Muench et al 2008;Robberto et al 2013;Schneider et al 2013). It contains the nearest massive star-forming cluster to Earth, the Trapezium cluster (e.g.…”