A&A 443, 541-556 (2005)
DOI: 10.1051/0004-6361:20042397
À. Gras-Velázquez - T. P. Ray
Dublin Institute for Advanced Studies, 5 Merrion Square, Dublin 2, Ireland
Received 19 November 2004 / Accepted 11 August 2005
Abstract
We have analysed new infrared photometric data taken
by the Infrared Space Observatory, in combination with 2MASS data where available, of 12 weak-line T Tauri stars (WTTS),
belonging to different molecular clouds. A control study of 6 classical T Tauri stars
(CTTS) for comparison with IRAS data has also been made.
WTTS traditionally are not
expected to have any circumstellar material, but
we have found that
11 of the WTTS studied,
have a spectral energy
distribution that suggests the presence of reprocessing
circumstellar disks, albeit half of them with apparent inner "dust holes''.
The spectral energy distribution curves of all the stars
in our sample show infrared excess in all cases except one.
We have also searched for companions to these stars and studied their possible
contributions to the
infrared emission.
We find that
10 of the WTTS with excess infrared emission have companions
that may contribute measurably and, in some cases significantly,
at infrared wavelengths.
In the case of the binary systems,
the amount of excess due to the companion is still unclear
but it is unlikely they are the only source of all the
observed excess.
We give estimations of the excesses and masses of the stars and also
find their ages and radii to be in agreement with those expected for T Tauri stars.
Our results suggest there is a continuum in infrared excess properties from
CTTS to WTTS rather than a clear differentiation based on a somewhat arbitrary
EW(H)
criterion.
Key words: stars: formation - infrared: stars - stars: pre-main sequence - circumstellar matter - techniques: photometric
Circumstellar disks are common around low-mass (
)
pre-main sequence stars,
e.g. Meyer, et al. (1997), and references therein; Kenyon & Hartmann (1990). These disks emit most of their energy in the infrared.
The infrared emission is the result of the disk's reprocessing of the radiation emitted by the stellar photosphere,
see for example, Wood et al. (2002) or Chandler (1998) and in some cases, viscous accretion
that heats the disk (Kenyon & Hartmann 1987).
As a result, the presence of disks around pre-main sequence
stars can be detected by an excess in the infrared wavelengths over the spectral energy distribution (SED)
corresponding to the star's photosphere (Kenyon & Hartmann 1987).
Table 1: Pre-main sequence stars observed.
T Tauri stars are pre-main sequence (no older than 105-107 yr),
low-mass (0.2
M*/
2) stars generally divided in two
subgroups: classical T Tauri Stars (CTTS) and weak-line T Tauri Stars (WTTS), e.g. Martín (1998).
As strong H
line emission is believed to be an indicator of the presence of an accretion disk (see Kenyon & Hartmann 1990;
and
references therein), authors have
traditionally stated that CTTS are stars with H
equivalent widths, EW(H
), greater than 10 Å and
large infrared excesses (indicative of circumstellar disks),
while WTTS have EW(H
)
10 Å and almost no excess (Alcalá et al. 1993).
This fact has led to the
suggestion that
WTTS are more evolved CTTS, e.g. Duvert et al. (2000).
More recently, categorization by fixed EW(H
)
has been questioned
and a weak dependence of the EW(H
)
borderline value on spectral type has been invoked (Martín 1998).
Thanks to the improved sensitivity and angular resolution of the Infrared Space Observatory (ISO) over the Infrared Astronomical Satellite (IRAS), ISO could detect much fainter infrared emission from Young Stellar Objects (YSOs). In particular we were able to obtain infrared photometry of a number of T Tauri stars at wavelengths for which they have not been previously observed.
Another characteristic of the formation of low-mass stars seems to be a high probability of them
being born in multiple systems (Günther & Kley 2002; Geoffray & Monin 2001). The aperture of ISO's photometer,
ISOPHOT, ranged from 10
to 120
for the observations referred to here. Therefore, any infrared excess
could potentially derive from an embedded companion (Chelli et al. 1988)
and we investigate that possibility here.
Using UV, optical and near-infrared data from the literature and the 2MASS and DENIS surveys, along with our new ISOPHOT photometry, we have constructed spectral energy distributions for 12 WTTS and 6 CTTS to search for infrared excesses, and where detected, to examine if this emission could be attributed to a disk around the primary target. With this aim in mind, we have also checked for companions and tried to assess their likely contrbution to the excess. The CTTS were included as a control sample for comparison with IRAS data. The ISO data also helps to improve their SEDs for modelling purposes.
Finally, using a H-R diagram with evolutionary tracks and isochrones from Palla & Stahler (1999), we have obtained the masses and ages for all the stars of our sample.
In this paper we present: in Sect. 2, the justification for our selected sample and technique used to reduce the data; Sect. 3, the procedure to obtain the SED and IR excesses and the complete list of stars with notes discussing particular problems encountered; Sect. 4, the discussion of the IR excesses, masses and ages calculated; and in Sect. 5, a summary of the results obtained. In the Appendix one can find the reduced ISO data as well as optical photometry obtained in La Palma for this paper. A further paper (Gras-Velázquez et al. 2005) will be devoted to detailed modelling of the SEDs in terms of flared disks and the different stars in each system.
Table 2: References for the uncorrected photometry used in Figs. 1 to 6.
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Figure 1:
SEDs of T Cha, Sz 68 and RU Lup. The photometry has been corrected
for extinction using the corresponding optical extinction
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The WTTS and the CTTS were largely chosen
from the Lupus, Ophiuchi and Serpens star forming regions.
These stars were selected from the Herbig-Bell Catalog (HBC) according to
their H
emission. A list of the stars, with their coordinates can be found in Table 1.
The corresponding IRAS point sources are also included, where known.
The infrared photometry was carried out using the multi-band, multi-aperture photometer PHT-P of ISOPHOT (PHT03), the
imaging photo-polarimeter on ISO. Observations for each star were
made with 9 filters, with central wavelengths (FWHM width)
of 4.8 (1.55), 7.7 (0.84), 10 (1.86), 12 (6.51), 12.8 (2.33),
15 (2.86), 20 (9.43), 60 (25.48) and 100 (40.15) m.
For the first five wavelengths the aperture used was 10
,
while for the 15 and 20
m filters
it was 23
and for the 60 and 100
m filters 120
.
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Figure 2: SEDs (cont.) of EX Lup, Sz 124 and ROX 2, as in Fig. 1. |
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The data was reduced using PIA (ISOPHOT's Interactive Analysis package) V10.0 following the Ramps Pattern Mode for Chopped Measurements and applying the standard procedures given in the manual (Gabriel et al. 1996). The reduced ISO photometry can be found in Appendix A.
The positive flux offset seen in some SEDs at 12.8 m and a negative
offset at 20
m,
are not special features, but
systematic flux offsets reported in the ISO handbook for these filters
which we have left unaltered here.
In the SEDs of the stars T Cha, Sz 68 and V536 Aql,
the flux obtained at 4.8 m
appears somewhat less than that from
M-band ground-based photometry.
For T Cha, we have compared this flux at 4.8
m with
those from ground-based photometry and ISO's
multi-aperture photometric observations (PHT04),
and believe the
differences are due to temporal variability
rather than an instrumental effect.
This variability in the near-infrared was
already pointed out by Alcalá et al. (1993).
The flux in the M band for Sz 68 and V536 Aql,
was taken from Geoffray & Monin (2001).
We believe the discrepancy at 5
m for these two stars,
is due also to variability, like in the case of T Cha.
Furthermore, for T Cha, we also have
MSX photometry at 8.3
m (Kraemer et al. 2003)
which confirms the ISO results at
7.7
m (see Fig. 1, cross at 8.3
m).
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Figure 3: SEDs (cont.) of DoAr 24, DoAr 24E and SR 12, as in Fig. 1. |
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The rest of the photometry included in the SED curves, was taken from different authors (see the complete list of references in Table 2) as well as the 2MASS and DENIS surveys (the full compilation of the photometry used for the SEDs can be found in Appendix B). For the stars CoKu Ser G1, CoKu Ser G7, V536 Aql and MacC H3, we obtained some photometric data from observations taken in La Palma in November 2003, with the Wide Field Camera on the Isaac Newton Telescope. This was reduced using the astronomical source extractor (SExtractor) from Bertin & Arnouts (1996) and corrected for airmass and exposure time. This latter photometry can also be found in Appendix A.
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Figure 4: SEDs (cont.) of ROX 31, Wa Oph/4 and Wa Oph/6, as in Fig. 1. |
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Figure 5: SEDs (cont.) of IX Oph, V1725 Oph and CoKu Ser G1, as in Fig. 1. |
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Figure 6: SEDs (cont.) of CoKu Ser G7, V536 Aql and MacC H3, as in Fig. 1. |
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We present SED graphs (Figs. 1 to 6) for our sample
in which we have combined: (squares)
optical (UBVRI) and near-infrared (JHKL) photometry from
previous papers and the 2MASS and DENIS surveys,
corrected for extinction using the most reliable
value for
(when consistency between 2MASS and the JHK
photometry presented in the literature was found, L and M-band
photometry were also taken from the same paper, if available);
(diamonds) new ISO photometry reduced by us for this paper;
(x's) IRAS values when available obtained from SIMBAD and Weaver & Jones (1992);
and (continuous curve) the black body distribution representing the stellar
photosphere, dependent on the spectral type.
The crosses and discontinuous curves
are the corresponding photometry and black body
when a different temperature
or an alternative extinction, was suggested in the literature
(see details for each case in the corresponding notes on individual objects).
The discontinuous straight line,
present in Sz 68, as an example,
represents the expected SED from a geometrically-thin, optically thick reprocessing disk viewed face-on
(
-4/3 at
2.2
m, Hillenbrand et al. 1992).
This line has been normalized to the flux at the J-band, as emission at this wavelength is considered to come
only from the star, for flat disks without dust holes.
The flatter slope we typically find in the infrared energy distribution is more
in agreement with flared reprocessing disk models as suggested by
Kenyon & Hartmann (1987), although a more exhaustive comparison remains to be done (Gras-Velázquez et al. 2005).
The combined SEDs of the binary systems for which we have NIR photometry for the companion can be found in Figs. 7 to 14.
We have assigned w (WTTS) or c (CTTS) to the stars in Table 3
adopting the classification scheme suggested by Martín (1998),
with the EW(H)
threshold depending on the spectral type.
Stars with the following EW(H
) are considered WTTS:
EW(H)
5 Å (for K-type stars)
EW(H)
10 Å (for M0-M2 stars)
EW(H)
20 Å (for later M stars)
Note that stars with their names underlined in the SED graphs are CTTS.
The visual extinction (
)
was obtained assuming
= RV
EB-V (Chini & Wargau 1998), where EB-V is the B-V colour excess.
The adopted colours and bolometric corrections are from
Reid (2002) and Lang (1992), respectively.
RV for members of the
Ophiuchi Dark Cloud was taken to be 4.2 if EV-K
1.0 (Teixeira & Emerson 1999; Rydgren 1980).
Otherwise the standard ISM value for RV
3.1, was assumed.
As it is difficult to know the exact
value of the extinction in a number of cases
we have taken the approach of assuming
the highest possible value of
for each star.
This procedure may lead to an overestimate of the photospheric
luminosity but the
infrared emission will remain largely unaltered. Having higher
stellar luminosity and the same infrared emission, decreases the
ratio between them. Hence, the calculated infrared excesses,
expressed in terms of the stellar luminosity,
will be lower limits (Finkenzeller & Basri 1987).
The excesses in the infrared emission have been calculated following the method already used by Cabrit et al. (1990),
where the infrared excess IR
is
the ratio of (
-
)
and
the luminosity of the star, L*.
is the infrared luminosity obtained by adding:
1. the flux calculated, from the wavelength stated for each star in Table 3 to the longest wavelength available,
by trapezoidal integration, and
2. the flux from the longest wavelength obtained by ISO for each star to infinite wavelengths
using the expression from Chavarría (1981), which supposes the emission at this wavelength to be the peak of a black body
curve.
is the luminosity of the black body representing the stellar photosphere, calculated over the same interval as
LIR, from integration of the
Rayleigh-Jeans part of the spectrum. The bolometric luminosity of the
star was obtained using L* =
(erg s-1), where BC is the bolometric correction
and
is the absolute visual magnitude.
It is important to note that the flat reprocessing geometrically thin disk model
permits an infrared excess no larger than 0.25 L* (Kenyon & Hartmann 1987; Hillenbrand et al. 1992).
In all cases, we also state the luminosity of the infraredexcess,
,
i.e.
-
,
in
.
For those stars with companions, we have also studied, the second star's photospheric contribution to the observed fluxes, if photometry and the temperature were available in the literature.
We present notes on the complete list of stars studied with comments on their spectral energy distributions, characteristics and calculations of the luminosities, infrared excesses, etc. Again we note that stars with their names underlined are CTTS.
This star was already studied by Alcalá et al. (1993), who consider
it a weak-line YY Orionis star.
YY Orionis stars are TTS with strong UV emission, quick photometric
and spectroscopic variability and possible mass accretion
onto the star (Alcalá et al. 1993).
There are ISO data presented here at more wavelengths (Fig. 1) than
Alcalá et al. (1993).
We have calculated the total IR
given in Table 3,
from 3.5
m to infinite wavelengths, extrapolating from the longest wavelength
obtained by ISO as explained earlier (100
m for this star).
In the SED (Fig. 1) of T Cha, we observed that the ISO points seem to decrease steadily
from L up to 20
m. As the photometry at 60 and 100
m could include emission
from a background source, we have also calculated the excess
from L to 20
m, and then extrapolated the flux from 20
m to infinite
wavelengths.
In this latter case, the
infrared excess decreases to 0.13 L* (0.22
).
Alcalá et al. (1993) believe the near-infrared excess could be due to an inner accretion disk despite this being a
WTTS.
In fact, it has been argued (Batalha et al. 1998) that T Cha
should be classified as a CTTS on the basis of the presence of this accretion from the disk.
No companion for this star has been reported in the literature.
This star is a WTTS and its SED (see Fig. 1) shows an
excess of 0.35 L* i.e.
1.60 ,
calculated from the L band.
Sz 68 has a companion at a projected separation of 390 AU ( 2
7) with a temperature
of 4000 K (Geoffray & Monin 2001). Plots of both stars' photometry are shown
in Fig. 7.
We have calculated the extinction towards the companion using the expression from Geoffray & Monin (2001)
-
), as we have not found photometry for the V and B bands.
Both stars seem to have excess emission at near-infrared wavelengths, which would indicate a
circumstellar disk around
each, as already suggested by Geoffray & Monin (2001). The new ISO measurements we present show quite a steeply rising infrared excess
starting at 10
m.
In principle this excess, suggesting the presence of an extended disk,
could come from either or both stars.
However it
seems too large to come only from Sz 68-B (Sz 68NW).
We obtain individually calculated luminosity excesses,
from 10
m onwards, of 1.36
(0.30 L*,A)
for Sz 68-A (i.e. if all the excess came from this star) and 1.51
(11.24 L*,B) if all
the excess belonged to Sz68-B.
We have not found any reference in the literature to the companion's H
emission that would tell us whether
the companion is a classical or a weak-line T Tauri star.
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Figure 7:
SED of Sz 68 A+B. Sz 68-A is represented by
a black body of 4955 K fitted to R (continuous line).
The squares are U to L band measurements of Sz 68-A, corrected
for an
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Sz 68-A itself is a 0
1 binary according to Ghez et al. (1997).
This, less-luminous, third component (Sz 68-C), with a K-band flux ratio of 6 (Ghez et al. 1997),
could be contributing
to the infrared excess observed as well.
Using the standard technique we were unable to calculate the extinction for RU Lup.
calculated from
-
)
yielded a negative value as well.
Therefore, we used
from Stempels & Piskunov (2002)
instead, which was obtained from line absorption.
The infrared excess from H to 4.8
m, in Fig. 1,
we thought could be due to variability and non-simultaneity of the
photometry, but comparing the 2MASS-JHK photometry with photometry from Gahm et al. (1993), crosses
in Fig. 1, we see there does not seem to be any variability at these wavelengths.
If the IR
is calculated from 4.8
m, which is where the infrared excess
intersects the black body curve of this star, instead of from 3.5
m, it goes down
from 0.68
(0.53 L*) to 0.61
(0.48 L*).
This star does not have any detected companion (Ghez et al. 1997).
We have not been able to calculate the star's extinction,
neither from EB-V, nor from ER-I,
both giving negative
.
Furthermore, it seems to be unknown (Herbig et al. 2001).
In Fig. 2, we have the photometry given
by Hughes et al. (1994), filled squares, fitted
by a 3802 K (M0.5) black body.
Therefore,
the luminosity of the star, uncorrected for extinction, with a spectral
type M0.5, is
0.47
.
The infrared excesses ratio is
0.35 L* (0.17
),
calculated from L.
We did not find any reference to a companion for this star in the literature.
Using a distance to the star of 125 pc and our calculated
of 0.22, we obtain a
luminosity of 0.21
.
The photometry from
ISO shows an excess (Fig. 2) that could come from a circumstellar disk. The infrared excess
calculated from 3.5
m is 0.81 L* (0.17
).
We have also corrected the UBV photometry using an
of 0.4 as given in Hughes et al. (1994), obtained
using the (R-I) color, but we have found
there is not much difference in the SED, the luminosity (0.25
)
or the infrared excess (0.68 L*,
0.17
)
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Figure 8:
SED of Sz 124 + Sz 124SE.
The black body curve of 3917 K belongs to Sz 124,
with the filled squares representing the star's photometry
corrected for an
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Sz 124 has a companion 13
6 away (Sz 124SE). We cannot obtain its temperature from the JHK photometry,
also from Hughes et al. (1994), as the extinction is unknown, but it appears (see Fig. 8)
that the excess observed by ISO at
12.8
m could come from either or both stars.
Due to the lack of information on the companion we cannot estimate its luminosity.
Bouvier & Appenzeller (1992) give a spectral type for this star between K3 and M0.
The latter spectral type is also given by Montmerle et al. (1983). In the SED graph (Fig. 2)
we have plotted both the black body distribution corresponding to a K3 and an M0 star. Both
black bodies seem to fit the UBV photometry. It can also be seen that the K3 black body distribution also fits the
near-infrared photometry and the flux at 12 m.
The extinction, however, rises from
= 3.32 (for M0) to
= 5.12 (K3) and therefore
the UBV photometry could be overdereddened. The infrared excesses found are
2.20 L* for M0 and 0.91 L* for K3, which is a
of 2.23
,
in both cases.
Although we have not included it in the SED,
we have also studied the case in which
= 5.9, given by Bouvier & Appenzeller (1992) (calculated using the V-Rcolour excess),
and spectral type K3, but the fit to the UBV photometry is very poor.
The infrared excess seems to appear at
12
m.
It would be possible for this emission to come from
the companion found 0
41 away by Barsony et al. (2003) and references therein.
This companion would have a flux at the K band of 0.57
Barsony et al. (2003).
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Figure 9:
SED of the system DoAr 24E A+B.
The continuous line is the photosphere of DoAr 24E-A:
a black body of 5236 K fitted to R;
the filled squares represent
the corrected photometry of the star.
The filled circles are the photometry given by Chelli et al. (1988),
except for J from Ageorges et al. (1997),
for the companion, not corrected for extinction.
Full diamonds are ISO measurements.
Crosses are IRAS measurements.
Empty triangles are photometry at 10 and 20 ![]() |
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From Bouvier & Appenzeller (1992) we have a spectral type of K5. There is an accuracy of 2 subclasses,
so we have also included in Fig. 3, the black body of a K3 star,
which fits the near-infrared photometry better. There is a
corresponding decrease
in the infrared excess from 2.17 L* (3.42
)
to 1.48 L* (2.34
).
If the extrapolation to infinite wavelength is done from 20
m,
the excess decreases even more (to 0.05 L*, 0.12
,
for the K3
spectral type).
No companion is reported in the literature and the infrared emission seems to indicate the presence of a circumstellar disk.
Using the spectral type of K0 given by Bouvier & Appenzeller (1992) we obtain an extinction of
= 5.84,
with RV = 4.2 (filled squares and continuous line in Fig. 3).
If we use the extinction of
= 6.6, also from Bouvier & Appenzeller (1992)
and calculated from the (V-R) colour excess,
the black body passes through the 4.8
and 10
m ISO points but U and B appear to be over-corrected (crosses and discontinuous line in
Fig. 3). We obtain an excess of 0.47 L* (3.97
)
in the first case and 0.22 L* (3.82
)
in the second. If we do not include the flux observed at 60
m and extrapolate
from the flux at 20
m the excess decreases to 0.08 L* (0.68
).
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Figure 10: SED of the system SR 12 A+B. A is the photosphere of SR 12-A with the empty triangles representing the corrected photometry of the star. B is the photosphere of SR 12-B with the filled circles being the apparent JHKL photometry of the companion. The empty squares are the photometry observed for the whole system. The discontinuous line corresponds to the sum of the blackbody fits for the two stars. The diamonds correspond to the fluxes obtained with ISO. References for the photometry are given in Table 2, except for SR12-B and the whole system which are from Simon et al. (1987). |
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Chelli et al. (1988) suggest the infrared excess from L onwards is emitted by an infrared companion at 2
3.
They find L*(DoAr 24E-A) = 7.9
and L*(DoAr 24E-B) = 1.4
,
assuming all the flux at
3.5
m to come from the main star and the rest from the companion.
In Fig. 9 we have plotted (filled dots) the
photometry of the companion (Chelli et al. 1988), not corrected for extinction, alongside the SED of the main star.
2MASS photometry for the companion does not seem to be available. Although the presence of
a companion and its contribution to the observed photometry cannot be ignored, the dip in the new fluxes observed by
ISO and the increase in the infrared emission at longer wavelengths, seems to indicate the presence of a disk.
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Figure 11: SED of Wa Oph/4 A and B. The continuous line is the photosphere of Wa Oph/4-A: a K4 black body (4500 K) fitted to V; the filled squares represent the corrected photometry for Wa Oph/4-A. The filled circles are the uncorrected photometry of the companion, Wa Oph/4-B. The diamonds correspond to the fluxes obtained by ISO. The x's correspond to the fluxes obtained by IRAS for Wa Oph/4. References for the photometry of the primary are given in Table 2. The photometry of the companion is from DENIS (I-band) and 2MASS (J, H and K bands). |
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Figure 12:
SED of V1725 Oph (H![]() ![]() ![]() ![]() ![]() |
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Bouvier & Appenzeller (1992) state a slightly higher value than Cohen & Kuhi (1979),
for the EW(H). It is still, however, less than 10 Å, and therefore
according to the standard definition a WTTS.
The most recent paper (Bouvier & Appenzeller 1992) states
the spectral type to be between K4 and M2.5.
Previous papers give spectral types of M1 (Rydgren et al. 1976; Cohen & Kuhi 1979)
and M2.5 (Rydgren 1980). In the SED graph (Fig. 3)
we have included both the black body distribution corresponding to a K4 star and a M2.5 star. The K4 black body fits the near-infrared
photometry, and the flux observed at 12
m, better. The extinction, however, rises to
= 2.69,
from 0.46 for M2.5.
The infrared excess found if a spectral type of M2.5 is assumed
is 2.65 L* (2.4
). If K4 were to be adopted, there would
still be a significant infrared excess of 1.18 L* (2.4
).
Simon et al. (1987) found SR 12 to be a 0
30 binary star (
50 AU),
from K band lunar occultation
observations. In their paper, they present K band magnitudes for both components and flux ratios
for the J and H magnitudes. They suggest temperatures of
5000 K for SR 12-A and 2500 K for SR 12-B.
Although a black body with effective temperature of 5000 K
would fit the infrared
photometry, we find the spectral type of M2.5 (3428 K) to be better for all the photometry available (from U to L).
In Fig. 10, we have plotted the black body curves (normalized to go through K)
corresponding to SR 12-A (3428 K) and SR 12-B (2500 K).
It can be seen that the total infrared flux (at J, H and K) of the two stars,
is approximately fitted by the sum of the two black body curves (discontinuous line in Fig. 10),
as well as the flux obtained with ISO at 12
m. There is still a clear infrared excess but
only at the longest ISO wavelengths.
If we suppose the infrared emission to come from a circumbinary disk, we obtain
the disk luminosity 1.71
(with
being the sum of the luminosities of the two stars).
No other companion has been reported nearby but we believe there must be an
embedded infrared
companion present to explain the large infrared excess we find.
For this star we have found no data corresponding to 3.5 m, so the infrared excess has been
calculated from 4.8
m.
Using K7 from Bouvier & Appenzeller (1992), we obtain the same
(4.2) and L* (0.48
)
given in their paper.
Taking into account the
2 subclass error in the spectral type we found that even using K5 or M1 as the star's temperature,
the H and K points were not fitted by a black body. The only possibility was to make
= 5.5, maintaining K7.
In this case the black body passes through H, K and the flux observed at 4.8
m.
Then the infrared excess is 0.33 L*
(0.52
),
instead of the 1.15 L* value (0.55
)
found with
= 4.2.
We have also included this option in Fig. 4, although supposing
= 5.5 seems to over-correct the
UBV magnitudes.
Simon et al. (1987) observed a companion at a projected angular separation of 130
.
This companion
should not contribute to the infrared emission observed, but Barsony et al. (2003), and references therein, reported
this star to have a second companion 0
39 away.
The magnitude difference in the K-band between ROX 31 and this second
companion is very small (
= 0.3, according to
Ageorges et al. 1997).
It is difficult to say
whether the large IR
comes only from a circumstellar disk or also from the subarcsecond companion.
Walter (1986) assumes RV to be 3.1. We have also included in the graph (Fig. 4) the black body if
RV = 4.2. This seems to bring the black body closer to fitting the 4.8 and 12 m points and also fits
the near-infrared photometry.
If RV = 4.2, which gives an
nearer to the value found in Chavarría (2000) obtained from
Strömgren photometry,
the infrared excess would be 0.04 L* (0.10
),
i.e. there would be less than half as much infrared excess, but still enough to suggest the presence of a disk.
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Figure 13:
SED of the system CoKu Ser G1 (HBC 667) and HBC 666.
The black body curve belongs to CoKu Ser G1,
with the filled squares representing the star's photometry
(see references in Table 2)
corrected for an
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Figure 14: SED of the system V536 Aql A+B. A is the photosphere of V536 Aql-A: the squares represent the corrected photometry and the continuous line is a black body of 4000 K fitted to V. The filled circles are the uncorrected JHKL photometry of V536 Aql-B. The diamonds correspond to the fluxes obtained by ISO. The x's correspond to the fluxes obtained by IRAS. References for the photometry of V536 Aql-A are given in Table 2. The photometry of the companion is from Geoffray & Monin (2001). |
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According to Reipurth & Zinnecker (1993), Wa Oph/4 has a
companion 8
7 away. We have plotted both stars'
photometry in Fig. 11.
Jensen et al. (2004) detected and
measured polarized light from both stars
(the polarization angle tends to be either
parallel or orthogonal to the disk rotation axis).
Hence, they imply both stars in the system have disks, confirming the
interpretation that the infrared excess seen for Wa Oph/4 comes from
a disk around the WTTS (although
the infrared excess at longer wavelengths seen in Fig. 11
could include a contribution from both disks).
In the graph (Fig. 4), we have the corrected available U to K magnitudes and black body curve where:
1.
= 1.24, calculated using RV = 3.1;
2.
= 1.68, calculated using RV = 4.2;
3.
= 2.74, calculated by Chavarría (2000),
from their Strömgren photometry.
The infrared excess decreases from 0.96 L* (0.64
),
to 0.23 L* (0.62
), for cases 1 to 3.
The excess has been calculated from 4.8
m
although it seems to start around 1.65
m.
Photometry in the JHK bands appear to be better fitted by a black body
normalized to V and corrected for
= 2.74.
This star does not seem to have a companion and the infrared excess probably comes from a circumstellar disk, in line with it being a CTTS.
No more information about the star's spectral type was found
apart from the fact that it is of G type
(Covino et al. 1992). This star does not have any infrared excess
detected by ISO (Fig. 5).
We note that it has one of the lowest H
equivalent widths in
Table 3.
Reipurth & Gee (1986) present a range of values for B and V.
In the SED (Fig. 5),
we have plotted the averages corrected for extinction using our calculated
= 0.28
(crosses) and
= 1.08 (filled squares), obtained from Strömgren photometry by Reipurth & Gee (1986),
both fitted with black body distributions
for an M0.5 star.
It can be seen that if an extinction of
= 1.08 is used, the curve is closer to
the 4.8
m point. The luminosity of the
star and the infrared excess, have been calculated using the black body curve fitted to the average magnitudes with
= 1.08 (solid-line curve in the graph).
This WTTS has not been reported to be a binary star but Weaver & Jones (1992)
noted that the IRAS emission associated with HBC 659 (B62-H2),
30
away, could be from
V1725 Oph as well.
We have plotted the SEDs of both stars with
the ISO and IRAS fluxes in Fig. 12.
The infrared emission observed by ISO at
m could be including emission
from a disk around B62-H
2.
Reipurth & Gee (1986) give a spectral type for B62-H
2
of M2 and an EW(H
)
of 19 Å (it is considered to be a classical T Tauri star).
We find a luminosity for this star of 0.43
.
Table 3:
H
equivalent widths, T Tauri classification,
spectral types, effective temperatures and distances of the
stars studied as found in the literature and used to calculate the
stellar luminosities and infrared excesses.
CoKu Ser G1 is a 3
5 pre-main-sequence binary (Jensen et al. 1996).
The companion (HBC 666) has an EW(H
) = 14.4 Å (Cohen & Kuhi 1979), but no spectral type is given.
We have also obtained from La Palma photometry for the companion in the V, R and I bands (see Fig. 13).
The IRAS fluxes shown in Fig. 13 may include contributions from HBC 666,
CoKu Ser G1 and even CoKu Ser G2, another CTTS less than 30
away (Weaver & Jones 1992).
Although the presence of a disk is clearly inferred, it is difficult to say to which stars it belongs to.
For this star we have also used
from Cohen & Kuhi (1979) and we can see in Fig. 6, the
infrared excess seems to start from H. The excess calculated from 4.8
m appears to be large.
CoKu Ser G7 is situated in the middle of the Serpens Cloud Core and 2MASS detected several additional
infrared sources at distances 10
,
although no companion for this star has been reported
in the literature.
Assuming a large background contribution at 60 and 100
m, we have conservatively
calculated the infrared excess up to 20
m and extrapolate from this wavelength, obtaining an IR
of 4.53 L* (3.71
). Furthermore,
if only the shorter wavelengths infrared excess (up to the 7.7
m point) were from the circumstellar disk,
the IR
would be 0.65 L* (0.54
).
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Figure 15: H-R diagram with evolutionary tracks to estimate the masses and ages of the stars observed. Stars with their names underlined are CTTS. The others are WTTS. The ZAMS (thick continuous line) is from VandenBerg & Bridges (1984). The evolutionary tracks (thin continuous lines), isochrones (thin discontinuous lines) and birthline (thick discontinuous line) are from Palla & Stahler (1999). |
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V536 Aql is a binary star with the companion estimated to be 0
52 away (
100 AU), Ageorges et al. (1994).
In Fig. 14 we have plotted both stars' fluxes using JHKL
for V536 Aql-B from Geoffray & Monin (2001).
The companion could also have a disk and its infrared emission be included in the excess observed for
V536 Aql.
Hirth et al. (1997) and Mundt & Eislöffel (1998) observed outflows from this star, implying the clear presence of an accretion disk.
Table 4: List of known secondaries to the T Tauri stars in our sample.
Cohen & Kuhi (1979) give a H
equivalent width of 11.4 Å, and Fernández et al. (1995) of 23.7 Å. It
is therefore a CTTS.
Besides the black body appropriate to the calculated extinction (
= 0.53), we have included the
corresponding black body if
= 1.25
(Cohen & Kuhi 1979) in Fig. 6 (
obtained as explained in the notes for CoKu Ser G1).
If the latter extinction is the correct one, the luminosity of the
star increases to 3.56
(from 1.83
)
and the infrared excess decreases from
1.66 L* to 0.85 L*,
with an
in both cases of
3.03
.
From the spectral energy distributions of the 12 weak-line T Tauri stars studied and the results summarized in Table 3 (for the main stars) and Table 4 (for the companions), we see that:
On the other hand, all 6 CTTS studied have infrared excesses that seem to indicate the presence
of circumstellar disks. Of these, 4 also show dips in the SEDs at 10 m, as in the case of the WTTS.
The broad dips found in the near-infrared part of the SEDs can be explained by a gap in the inner part of the disks due to the presence of an embedded planet (Rice et al. 2003), or of a companion star (Marsh & Mahoney 1992). To determine the physical size of these gaps, modelling is required. Modelling the infrared emission of each star in the binary systems will determine the infrared excess from the circumstellar disks and the contribution from the companions (Gras-Velázquez et al. 2005), as well.
We have used the luminosities and effective temperatures of the stars to place them in a H-R diagram
(Fig. 15) with evolutionary tracks and isochrones from Palla & Stahler (1999).
From the H-R diagram we have estimated the masses and ages of the stars (see complete list
of results in Table 5).
Due to the uncertainties in both the temperatures and the luminosities,
these results are not precise,
although they confirm that all the objects studied are pre-main sequence
(ages
107 yr) low-mass stars (0.2
M*/
).
Furthermore, there does not seem to be any clear difference between the ages of
CTTS and WTTS, as already suggested by other authors, e.g. Walter (1986) or Stempels & Piskunov (2002).
It is also interesting to note that all the stars appear under the stellar birthline,
considered to be the upper boundary in the H-R diagram where the T Tauri stars first become visible after
the end of accretion of the envelope and begin their quasi-static contraction towards
the ZAMS (Stahler 1983,1988).
Also from the H-R diagram (see Fig. 15), we can see that the only WTTS we found with no infrared excess whatsoever, IX Oph, is one of the oldest stars in our sample.
Table 5: Estimated ages, masses and radii of the stars in our sample and the companions.
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Figure 16:
In a), b) and c),
![]() ![]() ![]() |
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Following Cabrit et al. (1990), we have plotted H
luminosity against the
infrared excess for the 9 WTTS with possible circumstellar disks (see Fig. 16).
Moreover in Fig. 16, we also show plots of
against
and EW(H
)
against IR
,
for the WTTS and
the CTTS in our sample, with the WTTS and CTTS from Cabrit et al. (1990).
We have calculated
approximately from the H
equivalent widths and the
magnitudes, using
= 4
from Corcoran & Ray (1998).
We have found the correlation coefficients in the four cases shown in Fig. 16 to be:
0.85 for
vs.
for our WTTS; 0.85 for
vs.
for all the WTTS;
0.72 for
vs.
for all WTTS and CTTS and 0.53 for EW(H
)
vs. IR
for all the TTS.
As 8 of our 9 WTTS plotted have companions, the
calculated
will be an upper limit (since if the contribution to the IR emission from the
companions where subtracted, the
would go down).
Hence, the position of
the 8 WTTS in graph c) (filled diamonds in Fig. 16) would
move to the left, increasing the coherence even more.
Even without shifting, there appears to be a good correlation between the
and the
but not between
EW(H
)
and IR
.
Moreover the
correlation coefficient found, are approximately the same as the coefficients deduced by
Cabrit et al. (1990). These correlations suggest that WTTS and CTTS form a
continuous spectrum and not two
distinct classes divided somewhat arbitrarily by their H
equivalent width.
Using photometric measurements taken by ISO, we have obtained spectral energy distributions of 6 CTTS and
12 WTTS all of which (with one exception) show an infrared excess.
We have found that these excesses could indicate the presence
of circumstellar disks around not only all CTTS,
as expected, but also 9 of the WTTS.
8 of these WTTS plus another two WTTS also have companions or nearby
stars that could contribute to the infrared excess observed,
however in most cases it seems unlikely they are the
dominant contributor.
Moreover, half of the disks show evidence for inner dust-holes around 7.7 or 10 m.
Using
photometry of the different stars in each system and modelling the IR excess
we intend to distinguish the
contribution to the IR emission from the companion
and from the disks (Gras-Velázquez et al. 2005). Furthermore, the study of the
characteristics of the different
disk-like structures in our sample will provide information of
the differences, if any, between disks around CTTS and WTTS.
The picture that emerges is one of a gradual transition in disk
properties, from classical to weak-line T Tauri stars. The division,
based on H
equivalent widths, is somewhat arbitrary. Moreover the WTTS and the
CTTS appear to be approximately coeval, suggesting that in some
cases disks simply evolve faster than others.
Why this should be so remains unknown.
Acknowledgements
A.G.V. warmly thanks N. Calvet, B. Merín and K. Wood for their comments and help and also acknowledges support from Enterprise Ireland. The authors also wish to thank F. McGroarty and D. Froebrich for their help. The research has been done using the SIMBAD Database and the ALADIN image server, both operated at CDS, Strasbourg, France.
In the following table we present:
a) The fluxes in Jy reduced for the stars in our sample, at each of the 9 ISOPHOT wavelengths, using PIA V10.0 and following the Ramps Pattern Mode (Gabriel et al. 1996).
b) Only the new B, V, R and I photometric magnitudes obtained from the observations of CoKu Ser G1, CoKu Ser G7, V536 Aql and MacC H3, taken in La Palma for this paper.
![]() ![]() ![]() |
[mag] | ||||||||||||
4.80 | 7.70 | 10.00 | 12.00 | 12.80 | 15.00 | 20.00 | 60.00 | 100.00 | B | V | ![]() |
![]() |
|
T Cha |
0.390 | 0.437 | 0.198 | 0.223 | 0.296 | 0.132 | 0.177 | 7.903 | 8.517 | ||||
Sz 68 |
0.219 | 0.456 | 0.152 | 0.508 | 0.809 | 2.676 | 2.737 | 14.483 | 26.801 | ||||
RU Lup |
0.178 | 0.140 | 0.526 | 1.053 | 0.510 | 2.228 | 2.803 | 10.017 | 7.645 | ||||
EX Lup |
0.105 | 0.104 | 0.188 | 0.089 | - | 0.396 | 0.272 | 3.197 | 2.490 | ||||
Sz 124 |
- | - | - | - | 0.176 | - | - | 1.224 | 5.040 | ||||
ROX 2 |
- | - | - | 0.032 | 0.218 | - | - | 16.303 | 37.887 | ||||
DoAr 24 |
0.198 | 0.063 | 0.159 | 0.232 | 0.284 | 0.157 | 0.367 | 16.237 | 72.034 | ||||
DoAr 24E |
0.980 | 0.604 | 1.057 | 1.874 | 2.568 | 2.408 | 2.300 | 40.975 | - | ||||
SR 12 |
- | - | - | 0.030 | 0.029 | - | - | 11.710 | 49.230 | ||||
ROX 31 |
0.168 | 0.065 | - | - | 0.268 | - | - | 1.880 | 10.230 | ||||
Wa Oph/4 |
0.190 | - | - | 0.035 | 0.321 | - | 0.370 | 0.586 | - | ||||
Wa Oph/6 |
0.821 | 0.757 | 0.861 | 1.390 | 1.906 | 0.613 | 1.251 | 3.896 | 5.484 | ||||
IX Oph |
0.227 | - | - | 0.025 | 0.236 | 0.024 | - | - | - | ||||
V1725 Oph |
0.045 | - | 0.053 | 0.085 | 0.137 | 0.062 | 0.062 | 2.424 | 7.814 | ||||
CoKu Ser G1 |
0.111 | - | 0.480 | 0.407 | 0.586 | 0.418 | 0.512 | 4.551 | 4.883 | - | 17.4 | 16.1 | 14.2 |
CoKu Ser G7 |
0.187 | 0.214 | 0.621 | 1.391 | 0.895 | 3.300 | 2.841 | 54.967 | - | - | - | 16.4 | 14.5 |
V536 Aql |
0.218 | 0.495 | 0.628 | 1.604 | 3.332 | 2.415 | 3.650 | 8.854 | 7.353 | 15.7 | 13.9 | 12.9 | 11.4 |
MacC H3 |
- | 0.066 | 0.359 | 0.089 | 0.333 | 0.090 | - | 0.909 | - | - | - | - | 13.2 |
References for the photometry in this table can be found in Table 2 for the main stars and in the captions of Figs. 7 to 14 for the companions.
[mag] | IRAS [Jy] at ![]() ![]() |
|||||||||||||
U | B | V | ![]() |
![]() |
J | H | K | L | M | 12 | 25 | 60 | 100 | |
T Cha | 13.56 | 12.65 | 11.31 | 10.51 | 9.73 | 8.96 | 7.86 | 6.95 | 5.86 | 5.39 | 0.58 | 1.74 | 6.81 | 6.46 |
Sz 68 | 12.47 | 11.58 | 10.31 | 9.56 | 8.80 | 7.57 | 6.87 | 6.48 | 6.07 | 5.40 | 2.58 | 4.08 | 7.11 | 22.61 |
RU Lup | 12.63 | 11.92 | 11.25 | 10.56 | 9.86 | 8.73 | 7.82 | 7.14 | 6.09 | - | 2.18 | 4.36 | 4.61 | 5.70 |
EX Lup | - | 13.07 | 12.34 | 11.67 | 10.88 | 9.73 | 8.96 | 8.50 | 8.05 | 7.54 | 0.80 | 1.10 | 1.25 | - |
SZ 124 | 16.08 | 14.81 | 13.33 | 12.38 | 11.46 | 10.29 | 9.63 | 9.44 | 9.31 | 9.63 | 0.10 | 0.14 | - | - |
ROX 2 | 18.90 | 17.60 | 15.40 | 13.90 | 12.30 | 9.89 | 8.75 | 8.38 | - | - | 0.20 | 0.23 | - | - |
DoAr 24 | 17.50 | 16.10 | 14.20 | 13.00 | 11.80 | 9.66 | 8.61 | 8.06 | 7.55 | - | - | - | - | - |
DoAr 24E | 17.80 | 16.80 | 14.60 | 13.06 | 11.48 | 8.97 | 7.50 | 6.57 | 5.59 | - | 5.24 | 5.91 | - | - |
SR 12 | 16.57 | 14.95 | 13.31 | 12.34 | 10.90 | 10.21 | 9.39 | 9.17 | 9.05 | - | - | - | - | - |
ROX 31 | - | 19.10 | 16.80 | 15.40 | 13.50 | 10.00 | 9.40 | 8.80 | - | - | - | - | - | - |
Wa Oph/4 | 17.25 | 15.42 | 13.52 | 12.20 | 10.99 | 9.024 | 7.930 | 7.526 | - | - | 0.62 | 0.91 | 1.08 | - |
Wa Oph/6 | 15.80 | 14.90 | 13.20 | - | - | 8.72 | 7.57 | 6.86 | - | - | 1.31 | 1.98 | 1.96 | - |
IX Oph | 13.62 | 12.80 | 11.46 | 10.66 | 9.88 | 8.57 | 8.00 | 7.72 | 7.20 | - | - | - | - | - |
V1725 Oph | - | 15.89 | 14.39 | - | - | 10.36 | 9.35 | 8.86 | - | - | - | - | - | - |
CoKu Ser G1 | - | - | - | - | - | 11.52 | 11.00 | 9.70 | - | - | 0.64 | 2.10 | 2.86 | - |
CoKu Ser G7 | - | - | 17.60 | - | - | 12.05 | 10.79 | 9.30 | - | - | 2.51 | 5.77 | 92.60 | 418.25 |
V536 Aql | - | - | - | - | - | 9.14 | 8.10 | 7.40 | 6.77 | 5.70 | 3.07 | 5.82 | 5.79 | 6.61 |
MacC H3 | 15.44 | 15.59 | 14.50 | 14.10 | - | 11.68 | 10.99 | 10.68 | - | - | 0.27 | 0.40 | 1.66 | 2.55 |
Sz 68-B | - | - | - | 13.61 | 12.58 | 11.13 | 10.18 | 9.47 | 8.81 | 8.70 | - | - | - | - |
Sz 124SE | - | - | - | - | - | 10.82 | 9.65 | 9.15 | - | - | - | - | - | - |
ROX 2-B | - | - | - | - | - | - | - | - | - | - | - | - | - | - |
DoAr 24E-B | - | - | - | - | - | 12.10 | 9.40 | 7.81 | 5.78 | - | - | - | - | - |
SR 12-B | - | - | - | - | - | 10.97 | 10.15 | 9.93 | - | - | - | - | - | - |
ROX 31-B | - | - | - | - | - | - | - | - | - | - | - | - | - | - |
Wa Oph/4-B | - | - | - | - | 13.92 | 11.24 | 10.14 | 9.51 | - | - | - | - | - | - |
B62-H![]() |
- | - | - | - | - | 11.72 | 10.62 | 10.17 | - | - | 0.40 | 1.00 | 3.43 | 17.18 |
HBC 666 | - | - | 20.40 | 19.30 | 17.40 | 11.58 | 11.12 | 9.61 | - | - | - | - | - | - |
V536 Aql-B | - | - | - | - | - | 10.89 | 9.38 | 8.71 | 7.94 | 6.30 | - | - | - | - |