A&A 443, 541-556 (2005)
DOI: 10.1051/0004-6361:20042397

Weak-line T Tauri stars: circumstellar disks and companions[*]

I. Spectral energy distributions and infrared excesses

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

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$\alpha $) criterion.

Key words: stars: formation - infrared: stars - stars: pre-main sequence - circumstellar matter - techniques: photometric

1 Introduction

Circumstellar disks are common around low-mass ($M\sim1$ $M_{\odot}$) 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 $\leq$ M*/$M_{\odot}$ $\leq$ 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$\alpha $  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$\alpha $ equivalent widths, EW(H$\alpha $), greater than 10 Å and large infrared excesses (indicative of circumstellar disks), while WTTS have EW(H$\alpha $$\leq$ 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$\alpha $) has been questioned and a weak dependence of the EW(H$\alpha $) 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 $^{\prime\prime}$ to 120 $^{\prime\prime}$ 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.

...degraphics[width=5cm,height=8.3cm,angle=-90,clip]{2397fg1c.eps} \par\end{figure} Figure 1: SEDs of T Cha, Sz 68 and RU Lup. The photometry has been corrected for extinction using the corresponding optical extinction $A_{\rm {V}}$ given in Table 3. In this figure, photometric points from the literature and the 2MASS survey are given as filled squares, ISO points as filled diamonds and IRAS points as black x's. A typical star plus flat reprocessing disk fit to the spectra is shown in the case of Sz 68 as a dashed line. The presumed spectral type is also listed. Stars with their name underlined are known CTTS. Other symbols used are explained in the notes for the individual objects.
Open with DEXTER

2 Observations

The WTTS and the CTTS were largely chosen from the Lupus, $\rho$  Ophiuchi and Serpens star forming regions. These stars were selected from the Herbig-Bell Catalog (HBC) according to their H$\alpha $ 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) $\mu $m. For the first five wavelengths the aperture used was 10 $^{\prime\prime}$, while for the 15 and 20 $\mu $m filters it was 23 $^{\prime\prime}$ and for the 60 and 100 $\mu $m filters 120 $^{\prime\prime}$.

\par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2...
...,height=8.3cm,angle=-90,clip]{2397fg2c.eps} }
\par\par\end{figure} Figure 2: SEDs (cont.) of EX Lup, Sz 124 and ROX 2, as in Fig. 1.
Open with DEXTER

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 $\mu $m and a negative offset at 20 $\mu $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 $\mu $m appears somewhat less than that from M-band ground-based photometry. For T Cha, we have compared this flux at 4.8 $\mu $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 $\mu $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 $\mu $m (Kraemer et al. 2003) which confirms the ISO results at 7.7 $\mu $m (see Fig. 1, cross at 8.3 $\mu $m).

\par\vspace{-0.2mm} {\includegraphics[width=5cm,height=8.3cm,angl...
...,height=8.3cm,angle=-90,clip]{2397fg3c.eps} }
\par\par\end{figure} Figure 3: SEDs (cont.) of DoAr 24, DoAr 24E and SR 12, as in Fig. 1.
Open with DEXTER

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.

3 Results

3.1 Spectral energy distributions

\par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2...
...,height=8.3cm,angle=-90,clip]{2397fg4c.eps} }
\par\par\end{figure} Figure 4: SEDs (cont.) of ROX 31, Wa Oph/4 and Wa Oph/6, as in Fig. 1.
Open with DEXTER

\par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2...
...,height=8.3cm,angle=-90,clip]{2397fg5c.eps} }
\par\par\end{figure} Figure 5: SEDs (cont.) of IX Oph, V1725 Oph and CoKu Ser G1, as in Fig. 1.
Open with DEXTER

\par {\includegraphics[width=5.0cm,height=8.3cm,angle=-90,clip]{2...
...,height=8.3cm,angle=-90,clip]{2397fg6c.eps} }
\par\par\end{figure} Figure 6: SEDs (cont.) of CoKu Ser G7, V536 Aql and MacC H3, as in Fig. 1.
Open with DEXTER

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 $A_{\rm {V}}$ (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 ( $\lambda F_{\lambda}$ $\sim$ $\lambda$-4/3 at $\lambda$ $\geq$ 2.2 $\mu $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$\alpha $) threshold depending on the spectral type. Stars with the following EW(H$\alpha $)  are considered WTTS:
EW(H$\alpha $$\leq$ 5 Å (for K-type stars)
EW(H$\alpha $$\leq$ 10 Å (for M0-M2 stars)
EW(H$\alpha $$\leq$ 20 Å (for later M stars)

Note that stars with their names underlined in the SED graphs are CTTS.

3.2 Approach to the data analysis

The visual extinction ( $A_{\rm {V}}$) was obtained assuming $A_{\rm {V}}$ = RV $\cdot$ 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 $\rho$ Ophiuchi Dark Cloud was taken to be 4.2 if EV-K $\geq$ 1.0 (Teixeira & Emerson 1999; Rydgren 1980). Otherwise the standard ISM value for RV $\simeq$ 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 $A_{\rm {V}}$ 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 $_{\rm exc.}$ is the ratio of ( $L_{\rm IR}$ -  $L_{\rm bb}$) and the luminosity of the star, L*. $L_{\rm IR}$ 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. $L_{\rm bb}$ 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* =  $3.02~\times~10^{35}~\times~10^{-0.4(BC+M{_{\rm v}})}$ (erg s-1), where BC is the bolometric correction and $M_{\rm v}$ 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, $L_{\rm exc.}$, i.e. $L_{\rm IR}$ - $L_{\rm bb}$, in $L_{\odot }$.

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.

3.3 Notes on individual stars in the sample

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.

T Cha

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 $_{\rm exc.}$  given in Table 3, from 3.5 $\mu $m to infinite wavelengths, extrapolating from the longest wavelength obtained by ISO as explained earlier (100 $\mu $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 $\mu $m. As the photometry at 60 and 100 $\mu $m could include emission from a background source, we have also calculated the excess from L to 20 $\mu $m, and then extrapolated the flux from 20 $\mu $m to infinite wavelengths. In this latter case, the infrared excess decreases to 0.13 L* (0.22 $L_{\odot }$). 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.

Sz 68 (HT Lup)

This star is a WTTS and its SED (see Fig. 1) shows an excess of 0.35 L*  i.e. 1.60 $L_{\odot }$, calculated from the L band.

Sz 68 has a companion at a projected separation of 390 AU ($\sim$ 2 $.\!\!^{\prime\prime}$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) $A_{\rm V}=3.76\cdot E(R_{\rm {c}}$- $I_{\rm {c}}$), 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 $\mu $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 $\mu $m onwards, of 1.36 $L_{\odot }$ (0.30 L*,A) for Sz 68-A (i.e. if all the excess came from this star) and 1.51 $L_{\odot }$ (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$\alpha $ emission that would tell us whether the companion is a classical or a weak-line T Tauri star.

\par {\includegraphics[scale=0.85,angle=-90,clip]{2397fg7.eps} }
\par\par\end{figure} 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 $A_{\rm {V}}$ of 1.09. Sz 68-B is represented by a black body of 4000 K fitted to R (discontinuous line) with $A_{\rm {V}}$ = 0.75. The filled circles are the corresponding photometric measurements of Sz 68-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 Sz 68-A are given in Table 2. The photometry of the companion is from Hughes et al. (1994) for the R and I bands, and Geoffray & Monin (2001) for J, H, K and L.
Open with DEXTER

Sz 68-A itself is a $\sim$0 $.\!\!^{\prime\prime}$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.

RU Lup (HD142560)

Using the standard technique we were unable to calculate the extinction for RU Lup. $A_{\rm {V}}$ calculated from $E(R_{\rm {c}}$- $I_{\rm {c}}$) yielded a negative value as well. Therefore, we used $A_{\rm {V}}$ from Stempels & Piskunov (2002) instead, which was obtained from line absorption. The infrared excess from H to 4.8 $\mu $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 $_{\rm exc.}$is calculated from 4.8 $\mu $m, which is where the infrared excess intersects the black body curve of this star, instead of from 3.5 $\mu $m, it goes down from 0.68 $L_{\odot }$ (0.53 L*) to 0.61 $L_{\odot }$ (0.48 L*).

This star does not have any detected companion (Ghez et al. 1997).

EX Lup (HD 325367)

We have not been able to calculate the star's extinction, neither from EB-V, nor from ER-I, both giving negative $A_{\rm {V}}$. 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 $L_{\odot }$. The infrared excesses ratio is 0.35 L* (0.17 $L_{\odot }$), calculated from L.

We did not find any reference to a companion for this star in the literature.

Sz 124 (Th 43)

Using a distance to the star of 125 pc and our calculated $A_{\rm {V}}$ of 0.22, we obtain a luminosity of 0.21 $L_{\odot }$. The photometry from ISO shows an excess (Fig. 2) that could come from a circumstellar disk. The infrared excess calculated from 3.5 $\mu $m is 0.81 L* (0.17 $L_{\odot }$). We have also corrected the UBV photometry using an $A_{\rm {V}}$ 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 $L_{\odot }$) or the infrared excess (0.68 L*, 0.17 $L_{\odot }$)

\par {\includegraphics[scale=0.85,angle=-90,clip]{2397fg8.eps} }
\par\par\end{figure} 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 $A_{\rm {V}}$ of 0.22. Full diamonds are ISO observations and x's IRAS. The filled circles correspond to the JHK photometry given by Hughes et al. (1994) for Sz 124SE, not corrected for extinction.
Open with DEXTER

Sz 124 has a companion 13 $.\!\!^{\prime\prime}$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 $\lambda$ $\geq$ 12.8 $\mu $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 $\mu $m. The extinction, however, rises from $A_{\rm {V}}$ = 3.32 (for M0) to $A_{\rm {V}}$ = 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 $L_{\rm exc.}$ of 2.23 $L_{\odot }$, in both cases. Although we have not included it in the SED, we have also studied the case in which $A_{\rm {V}}$ = 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 $\lambda$ $\geq$ 12 $\mu $m. It would be possible for this emission to come from the companion found 0 $.\!\!^{\prime\prime}$41 away by Barsony et al. (2003) and references therein. This companion would have a flux at the K band of 0.57  $K_{\rm ROX~2}$ Barsony et al. (2003).

\par {\includegraphics[scale=0.85,angle=-90,clip]{2397fg9.eps} }
\par\par\end{figure} 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 $\mu $m, from Chelli et al. (1988).
Open with DEXTER

DoAr 24 (ROX 10A)

From Bouvier & Appenzeller (1992) we have a spectral type of K5. There is an accuracy of $\pm$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 $L_{\odot }$) to 1.48 L* (2.34 $L_{\odot }$). If the extrapolation to infinite wavelength is done from 20 $\mu $m, the excess decreases even more (to 0.05 L*, 0.12 $L_{\odot }$, 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.

DoAr 24E (ROX 10B)

Using the spectral type of K0 given by Bouvier & Appenzeller (1992) we obtain an extinction of $A_{\rm {V}}$ = 5.84, with RV = 4.2 (filled squares and continuous line in Fig. 3). If we use the extinction of $A_{\rm {V}}$ = 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 $\mu $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  $L_{\odot }$) in the first case and 0.22 L* (3.82 $L_{\odot }$) in the second. If we do not include the flux observed at 60 $\mu $m and extrapolate from the flux at 20 $\mu $m  the excess decreases to 0.08 L* (0.68 $L_{\odot }$).

\par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg10.eps} }
\par\par\end{figure} 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).
Open with DEXTER

Chelli et al. (1988) suggest the infrared excess from L onwards is emitted by an infrared companion at $\sim$2 $.\!\!^{\prime\prime}$3. They find L*(DoAr 24E-A) = 7.9  $L_{\odot }$ and L*(DoAr 24E-B) = 1.4  $L_{\odot }$, assuming all the flux at $\lambda$ $\leq$ 3.5 $\mu $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.

\par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg11.eps} }
\par\par\end{figure} 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).
Open with DEXTER

\par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg12.eps} }
\par\par\end{figure} Figure 12: SED of V1725 Oph (H$\alpha $3) and B62-H$\alpha $2 (H$\alpha $2). The continuous line is the photosphere of V1725 Oph: a black body of 3802 K (M0.5) fitted to V; the filled squares represent the corrected photometry of the star. The discontinuous line is the photosphere of B62-H$\alpha $2: a black body of 3500 K fitted to J, with the filled circles being the uncorrected photometry of this second star. The diamonds correspond to the fluxes obtained by ISO. The x's correspond to the fluxes obtained by IRAS for B62-H$\alpha $2. These fluxes could also come from V1725 Oph (Weaver & Jones 1992). References for the photometry of V1725 Oph are given in Table 2. The photometry of the nearby star is from Reipurth & Gee (1986).
Open with DEXTER

SR 12 (ROX 21, V2247 Oph)

Bouvier & Appenzeller (1992) state a slightly higher value than Cohen & Kuhi (1979), for the EW(H$\alpha $). 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 $\mu $m, better. The extinction, however, rises to $A_{\rm {V}}$ = 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 $L_{\odot }$). If K4 were to be adopted, there would still be a significant infrared excess of 1.18 L* (2.4 $L_{\odot }$).

Simon et al. (1987) found SR 12 to be a $\sim$0 $.\!\!^{\prime\prime}$30 binary star ($\sim$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 $\mu $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 $L_{\rm binary}$ (with $L_{\rm binary}$ 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.

ROX 31

For this star we have found no data corresponding to 3.5 $\mu $m, so the infrared excess has been calculated from 4.8 $\mu $m. Using K7 from Bouvier & Appenzeller (1992), we obtain the same $A_{\rm {V}}$ (4.2) and L* (0.48 $L_{\odot }$) given in their paper. Taking into account the $\pm$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 $A_{\rm {V}}$ = 5.5, maintaining K7. In this case the black body  passes through H, K and the flux observed at 4.8 $\mu $m. Then the infrared excess is 0.33 L* (0.52 $L_{\odot }$), instead of the 1.15 L* value (0.55 $L_{\odot }$) found with $A_{\rm {V}}$ = 4.2. We have also included this option in Fig. 4, although supposing $A_{\rm {V}}$ = 5.5 seems to over-correct the UBV magnitudes.

Simon et al. (1987) observed a companion at a projected angular separation of $\sim$130 $^{\prime\prime}$. 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 $.\!\!^{\prime\prime}$39 away. The magnitude difference in the K-band between ROX 31 and this second companion is very small ( $\delta m_{K}$ = 0.3, according to Ageorges et al. 1997). It is difficult to say whether the large IR $_{\rm exc.}$ comes only from a circumstellar disk or also from the subarcsecond companion.

Wa Oph/4 (V2507 Oph)

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 $\mu $m points and also fits the near-infrared photometry. If RV = 4.2, which gives an $A_{\rm {V}}$ nearer to the value found in Chavarría (2000) obtained from Strömgren photometry, the infrared excess would be 0.04 L* (0.10 $L_{\odot }$), i.e. there would be less than half as much infrared excess, but still enough to suggest the presence of a disk.

\par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg13.eps} }
\par\par\end{figure} 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 $A_{\rm {V}}$ of 3.48. Full diamonds are ISO observations and x's IRAS. The filled circles correspond to the photometry of the companion HBC 666, not corrected for extinction, with V (20.4 mag), R (19.3 mag) and I (17.4 mag) from the observations taken in La Palma for this paper and J, H and K from 2MASS.
Open with DEXTER

\par {\includegraphics[scale=0.83,angle=-90,clip]{2397fg14.eps} }
\par\par\end{figure} 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).
Open with DEXTER

According to Reipurth & Zinnecker (1993), Wa Oph/4 has a companion $\sim$8 $.\!\!^{\prime\prime}$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).

Wa Oph/6 (V2508 Oph)

In the graph (Fig. 4), we have the corrected available U to K magnitudes and black body curve where: 1. $A_{\rm {V}}$ = 1.24, calculated using RV = 3.1; 2. $A_{\rm {V}}$ = 1.68, calculated using RV = 4.2; 3. $A_{\rm {V}}$ = 2.74, calculated by Chavarría (2000), from their Strömgren photometry. The infrared excess decreases from 0.96 L* (0.64 $L_{\odot }$), to 0.23 L* (0.62 $L_{\odot }$), for cases 1 to 3. The excess has been calculated from 4.8 $\mu $m  although it seems to start around 1.65 $\mu $m. Photometry in the JHK bands appear to be better fitted by a black body normalized to V and corrected for $A_{\rm {V}}$ = 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.

IX Oph

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$\alpha $ equivalent widths in Table 3.

V1725 Oph (B62-H$\alpha $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 $A_{\rm {V}}$ = 0.28 (crosses) and $A_{\rm {V}}$ = 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 $A_{\rm {V}}$ = 1.08 is used, the curve is closer to the 4.8 $\mu $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 $A_{\rm {V}}$ = 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-H$\alpha $2), $\sim$30 $^{\prime\prime}$ 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 $\lambda\geq 20$ $\mu $m could be including emission from a disk around B62-H$\alpha $2. Reipurth & Gee (1986) give a spectral type for B62-H$\alpha $2 of M2 and an EW(H$\alpha $) of 19 Å (it is considered to be a classical T Tauri star). We find a luminosity for this star of 0.43 $L_{\odot }$.

Table 3: H$\alpha $ 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

For CoKu Ser G1, we have used $A_{\rm {V}}$ = 3.48, Cohen & Kuhi (1979), determined from image-tube-scanner narrow band indices between (0.54  $\mu $m - $R_{\rm c}$) and (0.60  $\mu $m - $R_{\rm c}$), with R=3.1 for the reddening law, as we do not have the star's B magnitude. The second black body present in the graph (Fig. 5) corresponds to $A_{\rm {V}}$ = 4.02, calculated using $A_{\rm {V}}$ = 3.76 $\cdot$  $E(R_{\rm {c}}$ -$I_{\rm {c}}$), Geoffray & Monin (2001), which seems to fit the near-infrared photometry slightly better. In the second case, the luminosity of the star increases from 0.60 $L_{\odot }$ to 0.99 $L_{\odot }$ and the infrared excess decreases from 3.70 L* (2.21 $L_{\odot }$) to 2.24 L* (2.21 $L_{\odot }$).

CoKu Ser G1 is a 3 $.\!\!^{\prime\prime}$5 pre-main-sequence binary (Jensen et al. 1996). The companion (HBC 666) has an EW(H$\alpha $) = 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 $^{\prime\prime}$ away (Weaver & Jones 1992). Although the presence of a disk is clearly inferred, it is difficult to say to which stars it belongs to.

CoKu Ser G7

For this star we have also used $A_{\rm {V}}$ 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 $\mu $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 $\leq$10 $^{\prime\prime}$, although no companion for this star has been reported in the literature. Assuming a large background contribution at 60 and 100 $\mu $m, we have conservatively calculated the infrared excess up to 20 $\mu $m and extrapolate from this wavelength, obtaining an IR $_{\rm exc.}$ of 4.53 L* (3.71 $L_{\odot }$). Furthermore, if only the shorter wavelengths infrared excess (up to the 7.7 $\mu $m point) were from the circumstellar disk, the IR $_{\rm exc.}$ would be 0.65 L* (0.54 $L_{\odot }$).

\par {\includegraphics[scale=0.60,angle=-90,clip]{2397fg15.eps} }
\par\par\end{figure} 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).
Open with DEXTER

V536 Aql

We have calculated $A_{\rm {V}}$ for this star from the photometry taken in La Palma. Using this $A_{\rm {V}}$ = 1.43, we obtain a luminosity of 0.72 $L_{\odot }$ and we observe (Fig. 6) an infrared excess which starts after R and has a dip around the 7.7 $\mu $m point. We have also plotted the black body fit to the photometry now corrected for an $A_{\rm {V}}$ = 3.2 from Cohen & Kuhi (1979), calculated as mentioned earlier, that seems to go through B up to 4.8 $\mu $m. With this second extinction, the luminosity of the star goes up from 0.72 $L_{\odot }$ to 3.69 $L_{\odot }$, and the infrared excess decreases from 2.48 L* (1.79 $L_{\odot }$) to 0.47 L* (1.75 $L_{\odot }$).

V536 Aql is a binary star with the companion estimated to be 0 $.\!\!^{\prime\prime}$52 away ($\sim$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.

MacC H3

Cohen & Kuhi (1979) give a H$\alpha $ 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 ( $A_{\rm {V}}$ = 0.53), we have included the corresponding black body if $A_{\rm {V}}$ = 1.25 (Cohen & Kuhi 1979) in Fig. 6 ( $A_{\rm {V}}$ 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 $L_{\odot }$ (from 1.83 $L_{\odot }$) and the infrared excess decreases from 1.66 L* to 0.85 L*, with an $L_{\rm exc.}$ in both cases of 3.03 $L_{\odot }$.

4 Discussion

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:

Half of the SEDs of the WTTS with excess show a flux deficit at 7.7 or 10 $\mu $m suggesting the presence of a dust free hole in the inner portion of the disk (Calvet et al. 2002).

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 $\mu $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 $\leq$ 107 yr) low-mass stars (0.2 $\leq$ M*/$M_{\odot}$   $\leq 2$). 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.

\par {\includegraphics[scale=0.65,angle=-90,clip]{2397fg16.eps} }
\par\end{figure} Figure 16: In a), b) and c), $L_{\rm H\alpha }$ is in units of $L_{\odot }$. In d), EW(H$\alpha $) is in Å. In the four figures: filled diamonds are the WTTS from our sample with possible circumstellar disks, filled circles are the WTTS from Cabrit et al. (1990), empty diamonds are the CTTS from our sample and empty circles are the CTTS from Cabrit et al. (1990). The Pearson product-moment correlation coefficients found between the different magnitudes are: a) 0.85, b) 0.85, c) 0.72, d) 0.53.
Open with DEXTER

Following Cabrit et al. (1990), we have plotted H$\alpha $ 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 $L_{\rm H\alpha }$ against $L_{\rm exc.}$ and EW(H$\alpha $) against IR $_{\rm exc.}$, for the WTTS and the CTTS in our sample, with the WTTS and CTTS from Cabrit et al. (1990). We have calculated $L_{\rm H\alpha }$ approximately from the H$\alpha $ equivalent widths and the $R_{\rm c}$ magnitudes, using $L_{\rm H\alpha }$ = 4$\pi d^{2}$ $\cdot F_{R_{\rm {c}}}$$\cdot$ $W_{\rm H\alpha}$ from Corcoran & Ray (1998). We have found the correlation coefficients in the four cases shown in Fig. 16 to be: 0.85 for $L_{\rm H\alpha }$ vs. $L_{\rm exc.}$ for our WTTS; 0.85 for $L_{\rm H\alpha }$ vs. $L_{\rm exc.}$ for all the WTTS; 0.72 for $L_{\rm H\alpha }$ vs. $L_{\rm exc.}$ for all WTTS and CTTS and 0.53 for EW(H$\alpha $) vs. IR $_{\rm exc.}$ for all the TTS. As 8 of our 9 WTTS plotted have companions, the $L_{\rm exc.}$ calculated will be an upper limit (since if the contribution to the IR emission from the companions where subtracted, the $L_{\rm exc.}$ 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 $L_{\rm H\alpha }$ and the $L_{\rm exc.}$ but not between EW(H$\alpha $) and IR $_{\rm exc.}$. 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$\alpha $ equivalent width.

5 Conclusions

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 $\mu $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$\alpha $ 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.

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.

Appendix A: New photometry reduced for this paper

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.

  $S_{\nu}$ [Jy] at $\lambda$ [$\mu $m] [mag]
  4.80 7.70 10.00 12.00 12.80 15.00 20.00 60.00 100.00 B V $R_{\rm c}$ $I_{\rm {c}}$

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        


- - - 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

Appendix B: Photometry used for the SEDs from previous papers

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 $\lambda$ [$\mu $m]
  U B V $R_{\rm c}$ $I_{\rm {c}}$ 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$\alpha $2 - - - - - 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 - - - -

Note to Tables A and B: the photometry presented here is uncorrected for extinction.



Copyright ESO 2005