Issue |
A&A
Volume 513, April 2010
|
|
---|---|---|
Article Number | A38 | |
Number of page(s) | 6 | |
Section | Catalogs and data | |
DOI | https://doi.org/10.1051/0004-6361/200913956 | |
Published online | 21 April 2010 |
A deep optical/near-infrared catalogue of
Serpens![[*]](/icons/foot_motif.png)
L. Spezzi1 - B. Merín2 - I. Oliveira3,4 - E. F. van Dishoeck4,5 - J. M. Brown5
1 - Research and Scientific Support Department, European Space Agency
(ESA-ESTEC), PO Box 299, 2200 AG Noordwijk, The Netherlands
2 - European Space Astronomy Center, European Space Agency (ESA-ESAC),
PO Box Apdo. de correos 78, 28691 Villanueva de la Cañada, Madrid,
Spain
3 - California Institute of Technology, Division for Geological and
Planetary Sciences, MS 150-21, Pasadena, CA 91125, USA
4 - Leiden Observatory, Leiden University, PO Box 9513, 2300 RA Leiden,
The Netherlands
5 - Max Planck Institut für Extraterrestrische Physik,
Giessenbachstrasse 1, 85748 Garching, Germany
Received 23 December 2009 / Accepted 8 February 2010
Abstract
We present a deep optical/near-infrared imaging survey of the Serpens
molecular cloud. This survey constitutes the complementary optical data
to the Spitzer ``Core To Disk'' (c2d) Legacy survey in this cloud. The
survey was conducted using the wide field camera at the Isaac Newton
Telescope. About 0.96 square degrees were imaged in the R
and Z filters, covering the entire region where
most of the young stellar objects identified by the c2d survey are
located. The 26 524 point-like sources were detected in both R
and Z bands down to mag
and
mag with a
signal-to-noise ratio better than 3. The 95% completeness limit of our
catalogue corresponds to 0.04
for members of the Serpens star-forming region (age 2 Myr and
distance 260 pc) in the absence of extinction. Adopting the
typical extinction of the observed area (A
mag), we estimate a
95% completeness level down to
.
The astrometric accuracy of our catalogue is 0.4 arcsec with
respect to the 2MASS catalogue. Our final catalogue contains J2000
celestial coordinates, magnitudes in the R and Z
bands calibrated to the SDSS photometric system and, where possible, JHKS
magnitudes from 2MASS for sources in 0.96 square degrees in
the direction of Serpens. This data product has already been used
within the frame of the c2d Spitzer Legacy Project analysis in Serpens
to study the star/disk formation and evolution in this cloud. Here we
use it to obtain new indications of the disk-less population in
Serpens.
Key words: catalogs - stars: formation - stars: low-mass - stars: brown dwarfs - ISM: clouds - ISM: individual objects: Serpens
1 Introduction
The Spitzer Legacy Survey ``Molecular Cores to Planet Forming Disks'' (c2d; Evans et al. 2003) has offered a singular opportunity for a major advance in the study of star and planet formation. Thanks to its sensitivity and wavelength coverage, Spitzer allowed us to address for the first time long-standing challenges such as disk formation and dispersal, the physical and chemical evolution of the circumstellar material and, in particular, to probe the inner planet-forming region of disks on the basis of statistically significant samples (see, e.g., Lada et al. 2006).
One of the star-forming regions included in the c2d survey is the Serpens molecular cloud. Because of its proximity (260 pc; Straizys et al. 1996) and young age (2-6 Myr; Oliveira et al. 2009), this cloud is particularly well-suited to studies of very young low-mass stars and substellar objects. The c2d survey in Serpens has provided evidence of sequential star formation in this cloud progressing from SW to NE and culminating in the main Serpens Core with its cluster of Class 0 objects (Kaas et al. 2004; Harvey et al. 2007); moreover, the surface density of young stars in this region is much higher, by a factor of 10-100, than that of the other star-forming regions mapped by the c2dteam (Evans et al. 2009) and includes 22% of the c2d sources classified as ``transitional'' disks. This makes Serpens the best region for obtaining a complete, well-defined sample of multi-wavelength observations of young stars and substellar objects in a possible evolutionary sequence to build up a ``template'' sample for the study of disk evolution up to a few Myr within a single, small, well-defined region. To this aim, the c2d Team has conducted several surveys, from X-ray to millimetre wavelengths, and spectroscopic follow-ups of the newly discovered population of young stars in Serpens, making this cloud only the third star-forming region after Taurus and IC 348 for which such an unbiased dataset exists (Harvey et al. 2007; Goodman 2004; Oliveira et al. 2009; Enoch et al. 2007, 2010, in prep.).
In this paper we present the optical/near-infrared (NIR) imaging data collected within the frame of the c2d survey in Serpens. These data represent one of the critical ingredients to anchor the studies of envelopes and disks to the properties of the central stars, including those without infrared excess. Indeed, deep XMM-Newton data of the same field revealed a sample of new sources, mostly candidate weak-line T Tauri stars (WTTSs), half of which have no counterpart in other catalogues (Brown et al. 2010, in prep.). Moreover, Comeròn et al. (2009) recently reported on a large-scale optical survey of the Lupus star-forming complex, which, in combination with NIR data from the 2MASS catalogue, unveiled a large population of stars and brown dwarfs (BDs) that have lost their inner disks on a time-scale of a few Myr or less. This discovery stresses the important unknowns that persistin the observational characterisation of young very low-mass objects and in the time-scales and mechanisms for disk dissipation.
The outline of this paper is as follows: in Sects. 2 and 3 we describe the observations and data reduction procedure, with particular emphasis on the photometric completeness and astrometric accuracy of the final optical/NIR catalogue in Sect. 4 we discuss the use of this catalogue within the frame of the c2d Team's analysis in Serpens and investigate its disk-less population. Our conclusions are drawn in Sect. 5.
2 Observations
The imaging observations presented in this work were carried out from 13 to 17 May 2008 using the Wide Field Camera (WFC) at the 2.5 m Isaac Newton Telescope (INT), which is located at the Roque de Los Muchachos Observatory (La Palma, Spain). The data were collected by Ignas Snellen as part of an observing practicum for Leiden University astronomy students.
The WFC is a four-chip mosaic of thinned AR coated EEV
devices.
Each CCD has an useful imaging area of
pixels
with a pixel scale of 0.333 arcsec/pixel, covering a total
field of view
arcmin
with small gaps of
20''
between adjacent chips. The average CCD read-out noise and gain are
7 e- and 2.8 e-/ADU,
respectively.
A total of 3 fields were observed in the direction of Serpens
(RA = 1829
49
,
Dec = +01
14
48
), covering the entire region
where most of the young stellar objects (YSOs) identified by the
Spitzer c2d survey are located (Fig. 1). Images were
obtained through the R (
Å,
Å) and Z
(
Å,
Å) filters
approximately covering the Sloan Digital Sky Survey (SDSS) r'
and z' bands (Fukugita
et al. 1996). The total sky-area observed in each
filter is 0.96 square degrees. Each observation in each filter
was split into several individual exposures (ditherings), shifting the
telescope pointing by
1 arcmin
between consecutive exposures; this allows us to cover the gaps between
the CCDs and avoid saturation of bright sources in the field. The
exposure time for each dithering was 120 s in both the R
and Z bands. In order to recover the photometry for
bright sources saturated in these long-time exposures, a series of
short-time exposures (i.e. 10 s per dithering in both filters)
of the same sky-area was also performed. The summary of these
observations is reported in Table 1. A standard
Landolt field was also observed in both filters for absolute flux
calibration purposes (Sect. 3.3).
![]() |
Figure 1:
IRAS 100 |
Open with DEXTER |
Table 1: Journal of the observations.
3 Data reduction
The raw images were processed using the IRAF
mscred package and a number of scripts ad hoc
developed both under IRAF and under IDL
.
We followed the steps for the WFC data reduction pipeline (Irwin & Lewis 2001)
developed by the Cambridge Astronomical Survey Unit (CASU), responsible
for the processing and archiving of the dataset from the INT Wide Field
Survey (WFS; McMahon et al. 2001).
3.1 Pre-reduction
Since the bias level tends to vary, the images were first corrected for
overscan and trimmed using the bias and trim sections as specified in
the FITS headers. For each night in which observations for our program
were performed, twilight flat frames were then combined to obtain the
night master flat, which was then used to correct the science images.
The corrected images are essentially linear to 2% over the full range. Bad pixels and partial
columns have been replaced using the bad pixel mask files available
from the WFS homepage
.
The Z-band images suffer from significant sky fringes. In order to remove them, we subtracted from each Z-band image the fringing pattern frame available from the WFS homepage scaled by a specific factor to account for the amplitude of the fringes in the individual science frames.
3.2 Astrometry and co-addition of images
The astrometric calibration and relative flux scaling between
ditherings were obtained using the c-version of ASTROMETRIX (M. Radovich, private
comm.). This tool performs a global astrometric solution that takes
overlapping
sources falling on adjacent CCDs in different ditherings into account.
For each pointing, the astrometric solution was computed using the
USNO-B1.0 catalogue (Monet
et al. 2003) as a reference. Within the global
astrometry process, the astrometric solution was constrained for each
CCD by both the positions from the USNO-B1.0 catalogue and those from
overlapping sources in all the other CCDs.
The co-addition of the dithered images for a given filter and
pointing was performed using the SWARP tool (Bertin
2008). The final stacked image is a
frame where each pixel value is the median flux of the co-added
ditherings normalised to the total exposure time and relative to the
airmass and atmospheric transparency of the first frame in the
dithering set. The absolute astrometric precision of our images is
about 0.4 arcsec, slightly lower than RMS accuracy of the
USNO-B1.0 catalogue (0.2 arcsec); the astrometric precision
has been also confirmed by a cross-check with the 2MASS point-source
catalogue (Fig. 2).
The internal RMS, computed from overlapping sources in different
exposures, is within 0.05 arcsec, indicating the good performance of
ASTROMETRIX.
![]() |
Figure 2: Residuals of the coordinates obtained by us for the sources in the surveyed area in Serpens with respect to those from the 2MASS catalogue. |
Open with DEXTER |
3.3 Photometric calibration
Instrumental magnitudes were reported to the standard SDSS photometric
system (Fukugita et al. 1996).
To this aim, the Stetson's standard star field L 104 (Stetson 2000) was observed in the RZ
filters.
By using the IRAF package photcal, we first
performed the aperture photometry for the standard stars, obtaining
their instrumental magnitudes (r0
and z0) corrected for
atmospheric extinction and normalised to the exposure time.
Then, the transformation coefficients, namely zero point (ZP)
and colour term (c), from the WFC-INT system to the
SDSS standard system were determined by a linear fitting of the
following equations:
where r' and z' are the standard magnitudes of Landolt's stars in the SDSS system.
The mean transformation coefficients determined in our observing run are reported in Table 2.
Using these coefficients, instrumental magnitudes (see
Sect. 3.4)
for the observed sources in Serpens have been converted to the SDSS
photometric system, which is nearly an AB system. Thus, magnitudes in
our catalogue can be turned into flux densities using the correction
from SDSS zero points to AB zero points and the AB zero point flux
density:
correction ZPR = 0 mag
F0
r' = 2.7769E-12
correction ZPZ = 0.02 mag
F0 z'
= 1.3153E-12
Table 2: Mean photometric calibration coefficients for our WFC-INT observing run.
3.4 The catalogue extraction
The source extraction and photometry from each stacked image in each
filter were performed by using the 2.5 version of the SExtractor tool
by Bertin & Arnouts (1996).
SExtractor exploits the aperture photometry technique, which is the
faster and best approach for uncrowded fields such as the one
considered here. In particular, we adopted the SExtractor adaptive
aperture magnitudes (
), which are estimated from a
flexible elliptical aperture around each detected object; this method
is expected to give the most precise magnitudes for very faint objects
which may appear extended. The detection threshold was set in order to
select all the sources having a signal-to-noise ratio (
)
greater than 3. The background is locally estimated from a ring shaped
region surrounding the star.
The output catalogues contain for each source an identification number, right ascension and declination in degree at J2000, instrumental magnitudes and relative errors, and two SExtractor morphological parameters, namely the extraction flag (FLAGS) and the isophotal area above the threshold (ISOAREA_IMAGE). These last parameters were used to clean the catalogues from spurious detections, such as cosmic ray hits, bad pixels, saturated or truncated sources too close to the image boundaries, etc.
In Fig. 3
we show as an example the internal photometric errors of all the
point-like sources detected in our long-time exposures plotted against
the magnitude for the RZ filters; the relative
exponential fits are over-plotted. Table 3 summarises
the saturation limit and the limiting magnitude achieved at the 10,
5
and 3
level in each filter for both the long time exposures and the short
ones.
Our final catalogue contains celestial coordinates (RA and Dec
at J2000) and RZ photometry for each point-like
object detected in our survey above the 3
level. Each entry in the catalogue was further complemented with
near-infrared JHKS
photometry by cross-matching it with the
2MASS Point Source Catalog (limiting magnitude
;
Skrutskie et al. 2006).
A matching radius of 2 arcsec was defined, which appears to be
sufficient given that more than 90% of the matches corresponded to
differences between the 2MASS positions and those determined by us of
less than 1 arcsec. When more than one 2MASS source was found
within the 2 arcsec circle, the one closer to the position
derived from our observations was chosen as the counterpart.
The full catalogue is downloadable from http://cdsarc.u-strasbg.fr/viz-bin/Cat
![]() |
Figure 3: Photometric errors versus magnitudes and relative exponential fits for all the point-like sources detected in the 0.96 square degrees area surveyed in Serpens. Photometry is from our long-time exposures (Sect. 2). |
Open with DEXTER |
Table 3:
Number of stellar sources ()
detected in both filters above the 3
level and limiting magnitudes in each filter at 10
,
5
,
3
and 95% completeness level.
3.5 Completeness
The completeness of our catalogue was estimated in the standard way by inserting artificial stars into the images and recovering them using the same extraction procedure as for the real objects (Sect. 3.4); the fraction of recovered artificial objects provides a measure of the completeness.
We used the DAOPHOT II standalone package to perform the exercise (Stetson 1987). We first use the PSF task to extract from the R and Z mosaics the relative PSF models. Then we inserted in each mosaic 1000 artificial sources using the addstar task; this number should not alter the crowding statistics in the images significantly. The profile for the artificial sources was generated by using the relative PSF model, while their positions are randomly distributed over the entire area of the mosaic and their magnitudes range uniformly between the detection and the saturation limits in the relative filter (see Table 3).
Figure 4 shows the fraction of recovered artificial objects as a function of magnitude from both the deep and shallow mosaics for the R and Z filters. The corresponding magnitude limits at 95% completeness level (C=95%) are reported in Table 3.
![]() |
Figure 4: Completeness (C) plot for extraction of artificial stars from our ``deep'' and ``shallow'' mosaics for the R and Z bands. |
Open with DEXTER |
In the absence of extinction (AV=0),
assuming a typical age for Serpens members of 2-6 Myr (Oliveira et al. 2009), a
distance of 260 pc (Straizys
et al. 1996) and using the theoretical isochrones
and evolutionary tracks by Baraffe
et al. (1998) and Chabrier
et al. (2000) and the completeness limits from
Table 3,
our optical survey would be complete down to 0.04
at the 95% level, i.e. well below the hydrogen burning limit (
0.08
).
However, as shown by Harvey
et al. (2007) in their Fig. 2, the visual
extinction toward the area observed in Serpens has a typical value of
mag.
Adopting this extinction, we estimate a 95% completeness level down to
,
4 On the disk-less population in Serpens
The observations presented in this paper are part of the c2d complementary work in Serpens. The optical/NIR catalogue described in Sect. 3.4 has been merged with the existing X-ray to millimetre wavelengths observations collected by the c2d Team for Serpens (Harvey et al. 2007; Goodman 2004; Oliveira et al. 2009; Enoch et al. 2007, 2010, in prep.), in order to construct complete spectral energy distributions (SEDs) of the YSOs in the observed fields. This dataset allows us to anchor disk properties of the Serpens YSO sample to the mass, age, and evolutionary status of the central object, which is a critical point in the studies of envelopes/disks formation and evolution (see, e.g., Pascucci et al. 2009; Kundurthy et al. 2006; Meyer 2009). A number of papers based on the use of the c2d extensive dataset for Serpens and presenting results on disk evolution are in preparation.
As mentioned in Sect. 1, Comeròn et al. (2009) have recently identified a large population of young members of the Lupus dark cloud complex which seems to have lost their inner disks on a time-scale of a few Myr or less. This discovery poses the important question of whether the existence of such disk-less young stars is the outcome of specific star-forming conditions in Lupus or similar populations exist in other regions.
XMM-Newton data obtained in April 2007 and April 2008 of the
same field observed by the c2d survey in Serpens revealed a sample of
new sources, half of which have no counterpart in the c2d catalogue and
are mostly candidate WTTSs (Brown et al. 2010, in prep.). For 44% of the
objects in this sample, we find optical and NIR colours consistent with
those of young objects with no prominent IR excess. Indeed, they occupy
in the Z vs. R-Z
(Fig. 5,
upper panel) the same locus as the YSOs identified by the c2d survey (Harvey et al. 2007), which
corresponds to an age between 1 and 10 Myr according to pre-main
sequence (PMS) isochrones by Baraffe
et al. (1998) and Chabrier
et al. (2000) and is consistent with the ages of the
c2d YSOs found by Oliveira
et al. (2009). The isochrones have been matched to
the SDSS photometric system following the procedure described in
Appendix B by Spezzi
et al. (2007). On the J-H
vs. H-K diagram the c2d YSOs
follow, as expected, the dwarf stars locus with many of them presenting
IR excess with respect to this locus; the X-ray sources mainly
concentrate on the field dwarfs locus, as expected for objects with no
disk. For the remaining objects in the X-ray source sample we could not
perform this analysis because they are either saturated or not detected
in our optical/NIR survey, while a few of them are out of the observed
field.
![]() |
Figure 5:
Z vs. R-Z
and J-H vs. H-K
diagrams for the YSOs in Serpens selected by the c2d survey (circles)
and the optical/NIR counterparts of the X-ray sources identified by
(Brown et al. 2010, in prep.) (squares). Upper panel:
the lines are the PMS isochrones by Baraffe
et al. (1998) and Chabrier
et al. (2000) transformed by us into the SDSS
photometric system. The arrow represents AV=2
reddening vector (Weingartner &
Draine 2001). Lower panel: the solid
curve shows the relation between the colour indices for main sequence
stars (lower branch) and giants (upper branch), together with the
relative reddening bands (dashed lines). The dash-dot line is the
T Tauri star locus by Meyer
et al. (1997). The object magnitudes are derreddened
using the typical extinction in the observed area (
|
Open with DEXTER |
To further investigate the disk-less population in Serpens, we tried to
apply to our dataset the novel S-parameter method
by Comeròn et al. (2009),
which allows the identification of possible young stars and substellar
objects based on their optical/NIR photospheric fluxes, independently
of the display of signposts of youth, such as IR excess emission or
strong H
emission. The S-parameter method simultaneously
estimates the visual extinction (AV),
effective temperature (
)
and a wavelength-independent scaling factor (S),
containing the dependency on the actual distance and radius of the
star, by fitting a grid of stellar photosphere models to the observed
SED. Using the Galactic star counts model by Wainscoat
et al. (1992), Comeròn
et al. (2009) demonstrated that members of nearby
young star forming regions at a given temperature
(<4000 K) and within a restricted set of ages
(<20 Myr) are characterised by values of S
virtually unreachable by non-members of similar temperature, both
foreground dwarfs and background giants. This method is expected to
work reasonably well for the detection of cool populations associated
to star-forming regions located in the
100-300 pc distance range from the Sun
(see Sect. 5 by Comeròn
et al. 2009) and, indeed, it has been successfully
applied to a number of nearby star forming regions: Lupus (Comeròn et al. 2009),
Cha I (Lopèz Martì, private communication), Cr A (Lòpez Martì et al. 2010)
and Cha II, where it provides the same results as in Spezzi et al. (2007). We
applied the S-parameter method to the optical/NIR
dataset for Serpens; we find that in this case the S-parameter
histogram at any temperature range shows no clear separation between
the member candidates and the background/foreground contaminants and,
as a consequence, the method produces an unreliable sample of member
candidates, which is also not compatible with the XMM-detected sources
in the same area of the sky. There are recent indications (see
Sect. 2.3 by Merìn
et al. 2008) that Galactic models may fail at
reproducing stellar counts at low galactic latitude and, indeed,
Serpens lies very close to the galactic plane (
deg). Moreover,
Serpens is located at 260 pc from the Sun, i.e. at the limit
of the validity range of the S-parameter method.
Since all the other clouds on which the method has been tested are
closer to the Sun and have higher galactic latitude than Serpens, we
conclude that the unlucky combination of distance and position of this
cloud prevents the S-parameter method from giving
useful results.
5 Conclusions
We presented an optical/NIR catalogue (R and Z
filters) of 26 524 point-like sources in 0.96 square
degrees in the direction of Serpens down to .
These data were collected using the WFC camera at the INT within the
frame of the Spitzer c2d survey in Serpens. The catalogue was also
complemented with JHKS
photometry from 2MASS and has been merged with the existing X-ray to
millimetre wavelengths observations collected by the c2d Team for
Serpens to study the envelop/disk formation and evolution and its
dependency on the stellar properties. A number of paper based on this
comprehensive catalogue are now published or in preparation (Merìn
et al. 2010a,b, in prep.; Oliveira et al. 2010, in
prep.; Brown et al. 2010, in prep.).
In this paper we used the optical/NIR catalogue to investigate
the disk-less population in Serpens. Because of the distance and low
galactic latitude of this cloud, the S-parameters
method by Comeròn et al. (2009),
suitable for the identification of young objects independently of any
signature of youth, fails in distinguishing young cloud members from
field contaminants. However, a sample of new WTTS candidates has been
identified in Serpens on the basis of XMM-Newton observations. Our
optical/NIR photometry suggests a very young age (10 Myr)
and no NIR excess emission for about 44% of them, supporting their WTTS
nature.
This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by NASA and the National Science Foundation. We also acknowledge extensive use of the SIMBAD database, operated at CDS Strasbourg. We thank Ignas Snellen and the students from Leiden Observatory for taking these INT data in service time. We thank Mario Radvich for the concession of ASTROMETRIX. We are also grateful to F. Comerón, J.M. Alcalá, H. Bouy, B. Lopéz Martí, R. Jayawardhana and the Spitzer c2d Team for useful discussions and suggestions. We are also grateful to many others, in particular to Salvatore Spezzi.
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Footnotes
- ... Serpens
- Catalogue (in VizieR) is only available in electronic form at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr/viz-bin/Cat
- ... IRAF
- IRAF is distributed by NOAO, which is operated by the Association of Universities for Research in Astronomy, Inc., under contract to the National Science Foundation.
- ... IDL
- Interactive Data Language.
- ...
homepage
- http://www.ast.cam.ac.uk/ wfcsur/technical/pipeline/
- ... ASTROMETRIX
- See also: http://www.na.astro.it/ radovich/wifix.htm
- ...
density
- See http://www.sdss.org/dr6/algorithms/fluxcal.html.
All Tables
Table 1: Journal of the observations.
Table 2: Mean photometric calibration coefficients for our WFC-INT observing run.
Table 3:
Number of stellar sources ()
detected in both filters above the 3
level and limiting magnitudes in each filter at 10
,
5
,
3
and 95% completeness level.
All Figures
![]() |
Figure 1:
IRAS 100 |
Open with DEXTER | |
In the text |
![]() |
Figure 2: Residuals of the coordinates obtained by us for the sources in the surveyed area in Serpens with respect to those from the 2MASS catalogue. |
Open with DEXTER | |
In the text |
![]() |
Figure 3: Photometric errors versus magnitudes and relative exponential fits for all the point-like sources detected in the 0.96 square degrees area surveyed in Serpens. Photometry is from our long-time exposures (Sect. 2). |
Open with DEXTER | |
In the text |
![]() |
Figure 4: Completeness (C) plot for extraction of artificial stars from our ``deep'' and ``shallow'' mosaics for the R and Z bands. |
Open with DEXTER | |
In the text |
![]() |
Figure 5:
Z vs. R-Z
and J-H vs. H-K
diagrams for the YSOs in Serpens selected by the c2d survey (circles)
and the optical/NIR counterparts of the X-ray sources identified by
(Brown et al. 2010, in prep.) (squares). Upper panel:
the lines are the PMS isochrones by Baraffe
et al. (1998) and Chabrier
et al. (2000) transformed by us into the SDSS
photometric system. The arrow represents AV=2
reddening vector (Weingartner &
Draine 2001). Lower panel: the solid
curve shows the relation between the colour indices for main sequence
stars (lower branch) and giants (upper branch), together with the
relative reddening bands (dashed lines). The dash-dot line is the
T Tauri star locus by Meyer
et al. (1997). The object magnitudes are derreddened
using the typical extinction in the observed area (
|
Open with DEXTER | |
In the text |
Copyright ESO 2010
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