J/ApJ/725/2232 Deep NIR survey of the Pipe Nebula. II. (Roman-Zuniga+, 2010)
Deep near-infrared survey of the Pipe Nebula.
II. Data, methods, and dust extinction maps.
Roman-Zuniga C.G., Alves J.F., Lada C.J., Lombardi M.
<Astrophys. J., 725, 2232-2250 (2010)>
=2010ApJ...725.2232R 2010ApJ...725.2232R
ADC_Keywords: Extinction ; Interstellar medium ; Molecular clouds ; Surveys ;
Magnitudes ; Infrared sources
Keywords: ISM: clouds - infrared: ISM - stars: formation
Abstract:
We present a new set of high-resolution dust extinction maps of the
nearby and essentially starless Pipe Nebula molecular cloud. The maps
were constructed from a concerted deep near-infrared imaging survey
with the ESO-VLT, ESO-NTT, CAHA 3.5m telescopes, and 2MASS data. The
new maps have a resolution three times higher than the previous
extinction map of this cloud by Lombardi et al. (2006A&A...454..781L 2006A&A...454..781L)
and are able to resolve structures down to 2600AU. We detect 244
significant extinction peaks across the cloud. These peaks have masses
between 0.1 and 18.4M☉, diameters between 1.2 and 5.7x104AU
(0.06 and 0.28pc), and mean densities of about 104cm-3, all in
good agreement with previous results. From the analysis of the mean
surface density of companions we find a well-defined scale near
1.4x104AU below which we detect a significant decrease in structure
of the cloud. This scale is smaller than the Jeans length calculated
from the mean density of the peaks. The surface density of peaks is
not uniform but instead it displays clustering. Extinction peaks in
the Pipe Nebula appear to have a spatial distribution similar to the
stars in Taurus, suggesting that the spatial distribution of stars
evolves directly from the primordial spatial distribution of
high-density material.
Description:
A list of all fields observed and considered for final analysis can be
consulted in tablea1. The main observations of the survey were made
with the ISAAC and the Son of ISAAC (SOFI) near-infrared imagers,
mounted, respectively, at the UT3 8.2m unit of the VLT array at Cerro
Paranal and the 3.5m NTT at La Silla, both parts of the ESO in Chile.
The two observing runs were completed in the summer months of 2001 and
2002.
The Centro Astronomico Hispano Aleman (CAHA) 3.5m observations were
done with the OMEGA 2000 camera, which has a wide FOV of 15'. A total
of 21 fields, complementary to the ESO survey, were observed during
2007 June and 2008 June.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 35 220 CLUMPFIND-2D identifications in high-resolution
extinction maps of the Pipe Nebula
tablea1.dat 82 197 Near-infrared observations of Pipe Nebula fields
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See also:
B/eso : ESO Science Archive Catalog (ESO, 2012)
II/246 : 2MASS All-Sky Catalog of Point Sources (Cutri+ 2003)
J/ApJ/699/742 : Properties of cores in the Pipe Nebula (Rathborne+, 2009)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 5 A5 --- Reg Region name (Stem, Shank, Bowl or Smoke maps,
see figure 2)
7- 10 A4 --- PID Peak identification from RLA09 ([R/N]NNN) (1)
11 A1 --- m_PID [a-h] close peaks (2)
12 A1 --- n_PID [*] Note on PID (3)
14- 17 F4.1 mag Av Maximum extinction (4)
19- 23 F5.3 pc Req [0.022/0.146] Equivalent radius of the peak
25- 29 F5.3 Msun Mass [0.054/4.812] Mass of the extinction peak region
31- 35 F5.3 10+4cm-3 n [0.41/4.687] Average density of the peak
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Note (1): Peak identifications follow the numbering used in the list of
Rathborne et al. 2009, Cat. J/ApJ/699/742; <[RLM2009] NNNa> for
Simbad). Peaks identified with "N" were previously undetected.
Note (2): Peaks located by less than one Jeans length from a coincident
Rathborne et al. 2009, Cat. J/ApJ/699/742, position are listed with
the core number followed by letters (a, b, c, etc.), which list peaks
alphabetically from the largest to the smallest mass.
Note (3): An asterisk indicates when a peak in a group is also separated by less
than 0.12km/s in radial velocity with respect to the main position.
Note (4): Peak extinction values in this list are those listed by CLF2D for the
wavelet-filtered maps (which have a background value of zero).
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Byte-by-byte Description of file: tablea1.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- Inst Instrument used for observations (SOFI-NTT,
ISAAC-VLT, or OMEGA 2000-CAHA 3.5m)
11- 20 A10 --- Field Field identification
22- 32 A11 "YYYY/MMM/DD" Date Date of observation
34- 43 F10.6 deg RAdeg Center right ascension (J2000)
45- 54 F10.6 deg DEdeg Center declination (J2000)
56- 57 A2 --- F Filter (J, H, or Ks)
59- 62 F4.2 arcsec See Estimated seeing based on the average FWHM of
the stars detected in each field
64- 68 F5.2 mag Pmag [16.75/24.5] Peak of the observed magnitude
distribution
70- 82 A13 --- Map Corresponding figure number in large-scale
maps (figures 3-7) and atlas
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History:
From electronic version of the journal
References:
Roman-Zuniga et al. Paper I. 2009ApJ...704..183R 2009ApJ...704..183R
(End) Emmanuelle Perret [CDS] 10-Aug-2012