The COMPLETE Survey of Star-Forming Regions: Phase I Data

By N. Ridge, J. di Francesco, H. Kirk, Di Li, A. Goodman, Joao F. Alves, H. Arce, Michelle A. Borkin, P. Caselli, J. Foster and 7 more. 2006

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We present an overview of data available for the Ophiuchus and Perseus molecular clouds from Phase I of the COMPLETE Survey of Star-Forming Regions. This survey provides a range of data complementary to the Spitzer Legacy Program "From Molecular Cores to Planet Forming Disks." Phase I includes the following: extinction maps derived from the Two Micron All Sky Survey (2MASS) near-infrared data using the NICER algorithm; extinction and temperature maps derived from IRAS 60 and 100 μm emission; H I maps of atomic gas; 12CO and 13CO maps of molecular gas; and submillimeter continuum images of emission from dust in dense cores. Not unexpectedly, the morphology of the regions appears quite different depending on the column density tracer that is used, with IRAS tracing mainly warmer dust and CO being biased by chemical, excitation, and optical depth effects. Histograms of column density distribution are presented, showing that extinction as derived from 2MASS NICER gives the closest match to a lognormal distribution, as is predicted by numerical simulations. All the data presented in this paper, and links to more detailed publications on their implications, are publicly available at the COMPLETE Web site.

Subfields: Astronomy and Astrophysics, Instrumentation, Statistical and Nonlinear Physics

View Paper: https://www.semanticscholar.org/paper/a81d4adb82bf6754a77146e779a9eca38d20fbac

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Citations in the corpus

STAR FORMATION RELATIONS IN NEARBY MOLECULAR CLOUDS (2014, methodology): “They are also targeted in Herschel surveys covering 60 to 500 µm (André et al. 2011), and some have been studied in more detail in millimeter continuum emission (e.g., Enoch et al. 2009) and molecular lines (e.g., Ridge et al. 2006).”
THE STAR FORMATION RATE AND GAS SURFACE DENSITY RELATION IN THE MILKY WAY: IMPLICATIONS FOR EXTRAGALACTIC STUDIES (2010, background): “We can directly test this in two galactic clouds, Perseus and Ophiuchus, which both have 12CO J=1–0 and 13CO J=1–0 maps from the Five College Radio Astronomy Observatory (FCRAO) COordinated Molecular Probe Line Extinction Thermal Emission (COMPLETE) Survey of Star Forming Regions (Ridge et al. 2006)”
Gravity or turbulence? II. Evolving column density PDFs in molecular clouds (2011, methodology): “For instance, Ridge et al. (2006) used extinction data from the COMPLETE (COordinated Molecular Probe Line Extinction Thermal Emission) Survey of StarForming Regions, to argue that the gas in Ophiuchus and Perseus molecular clouds exhibits a lognormal N-PDF(see also Goodman et al. 2009).”
Comparing Star Formation on Large Scales in the c2d Legacy Clouds: Bolocam 1.1 mm Dust Continuum Surveys of Serpens, Perseus, and Ophiuchus (2007, unknown): “Large 13CO maps of Perseus and Ophiuchus observed with FCRAO at a resolution of 44′′ are publicly available as part of “The COMPLETE Survey of Star Forming Regions”7 (COMPLETE; Goodman et al. 2004; Ridge et al. 2006).”
A Spitzer Census of the IC 348 Nebula (2007, methodology): “The most useful sets of such dust and gas maps come from the publicly available COMPLETE project, which were published by Ridge et al. (2006).”
On the Reuse of Scientific Data (2017, background): “…is the COMPLETE (Coordinated Molecular Probe Line Extinction Thermal Emission Survey of Star Forming Regions) Survey, that integrated new observations with datasets retrieved from public repositories of astronomical observations that cover same regions of the sky (Goodman 2004; Ridge et al. 2006).”
Cold Dark Clouds: The Initial Conditions for Star Formation (2007, methodology): “Ridge et al. (2006) find lognormal distributions for the number of pixels as a function of extinction in both Perseus and Ophiuchus, a distribution that is in agreement with the expectation from turbulent models of cloud formation (Vazquez-Semadeni 1994; Ostriker, Stone & Gammie 2001).”
Theory of Star Formation (2007, background): “…2001), distributions of extinction follow log-normal functional forms to an excellent approximation; distributions of integrated intensity from molecular lines, on the other hand, are not log-normal (Ridge et al., 2006), presumably due to a combination of chemistry and/or optical depth effects.”
KINEMATIC AND SPATIAL SUBSTRUCTURE IN NGC 2264 (2015, methodology): “The left panel shows the positions of all the radial velocity targets overplotted on the corresponding 13CO intensity map from Ridge et al. (2006) for comparison.”
Characterizing Young Brown Dwarfs Using Low-Resolution Near-Infrared Spectra (2006, background): “Oph 1622 2405A and Oph 1622 2405B show no sign of foreground reddening, even though the AV of the Ophiuchus cloud is 4.5 mag (Ridge et al. 2006) at the position of Oph 1622 2405A and Oph 1622 2405B, which makes it unlikely that Oph 1622 2405A and Oph 1622 2405B lie behind the Ophiuchus/Upper…”
THE SPITZER c2d LEGACY RESULTS: STAR-FORMATION RATES AND EFFICIENCIES; EVOLUTION AND LIFETIMES (2008, methodology): “For Perseus, Serpens, and Ophiuchus, J. E. Pineda (pers. comm. 2008) has provided the mean and median linewidths for the ensemble of spectra in the COMPLETE maps (Ridge et al. 2006), and the average and difference of the median and mean are given in Table 1 as the value and uncertainty.”
CO Isotopologues in the Perseus Molecular Cloud Complex: the X-factor and Regional Variations (2008, methodology): “The Shell region is essentially the same as the shell-like feature discussed in Ridge et al. (2006a).”
FILAMENTARY STRUCTURE OF STAR-FORMING COMPLEXES (2009, methodology): “8 Figure 6 shows the IC348 region in the E part of the Perseus complex, in contours of integrated intensity of the J=1-0 line of 13CO (Ridge et al 2006), with associated YSOs based on Spitzer Space Telescope observations (Muench et al 2007).”
Molecular Clouds in the Milky Way (2015, background): “The 13CO J = 1–0 line is sufficiently bright to allow mapping of its distribution over large angular scales along the Galactic plane and in nearby star-forming regions (Bally et al. 1987, Yonekura et al. 1997, Lee et al. 2001, Jackson et al. 2006, Ridge et al. 2006, Narayanan et al. 2008).”
An Ammonia Spectral Atlas of Dense Cores in Perseus (2007, methodology): “The velocity window comes from the COMPLETE observations of 13CO toward the Perseus cloud (Ridge et al. 2006).”
The Large- and Small-Scale Structures of Dust in the Star-forming Perseus Molecular Cloud (2006, methodology): “…authors suggesting that the system is composed of two distinct clouds at different distances - e.g., Ungerects & Thaddeus (1987); Goodman et al. (1990); C̆ernis & Straizys (2003); Ridge et al. (2006a); with the closer cloud being an extension of Taurus and the further a shell-like structure.”
Structural Analysis of Molecular Clouds: Dendrograms (2008, methodology): “L1448 COMPLETE Data Our primary observational data set for demonstrating the dendrogram method is a section of the Coordinated Molecular Probe Line Extinction Thermal Emission6 survey’s13CO map of Perseus (Ridge et al. 2006), centered on the L1448 starforming region.”
DIRECT OBSERVATION OF A SHARP TRANSITION TO COHERENCE IN DENSE CORES (2010, unknown): “6 Full description and analysis of all of the COMPLETE Survey’s (Ridge et al. 2006) GBT NH3 maps of Perseus cores, including B5, will be presented in Pineda et al., in preparation 7 http://gbtidl.nrao.edu/ 03h48m0s 47m50s 40s 30s 20s 10s 32°44′0′′ 46′0′′ 48′0′′ 50′0′′ 52′0′′ 54′0′′ 56′0′′ RA…”