1 Henning et al. (1993A&A...276..129H) measured a 1.3mm flux. We included this
 1  star for the purpose of checking calibration of ISO fluxes.
 2 Indistinguishable from the nearby reflection nebula in the IRAS beam.
 2  At 60{mu}m, our observations indicate a point source. At 100{mu}m, we are
 2  only able to place an upper limit to the flux.
 3 Henning et al. (1993A&A...276..129H) measured a 1.3mm flux. At 60{mu}m, our
 3  observations indicate a point source. At 100{mu}m, the data appear to be
 3  contaminated by flux from the nearby B-type star HD 97048, and we give only
 3  an upper limit.
 4 Another TTS, CHX 15a falls on one of the source-frame pixels. IRAS detected
 4  flux from both objects, and we give an upper limit to the contribution from
 4  WY Cha. At 60{mu}m, the total fluxes agree with the IRAS value; at 100{mu}m,
 4  cirrus confusion is very high.
 5 Originally identified as the source of the far-IR emission detected by IRAS
 5  at this position. Subsequent X-ray studies questioned this association, and
 5  Walter (1992AJ....104..758W) considered nearby CHX 18N (also WTTs,
 5  separation 24) to be the IR source. In our ISO observations, the two stars
 5  fall on different pixels in the source frame. Both pixels show detected
 5  emission, and it seems that each star contributes part of the far-IR
 5  emission.
 6 This star has surrounding nebulosity. It appears to be a point source
 6  at 60{mu}m but at 100{mu}m appears either extended or confused with the
 6  nebulosity.
 7 Henning et al. (1993A&A...276..129H) measured a 1.3mm flux. Our measurements
 7  at 60 and 100{mu}m are significantly lower than IRAS co-added data. Evidence
 7  for either extension or nebulosity confusion at 100{mu}m.
 8 One of the X-rayselected WTTs (Alcala et al., 1995, Cat. <J/A+AS/114/109>),
 8  and it was one of the few confirmed as PMS by detection of lithium
 8  (Covino et al., 1997A&A...328..187C).
 9 X-rayselected WTTs (Walter et al., 1994AJ....107..692W). It appears quite
 9  extended in our data at both wavelengths.
10 Hartigan (1993AJ....105.1511H) notes that this source has essentially
10  disappeared since its first detection.
11 IRAS lists no data for either VW Cha or Sz 23 due to the proximity of the
11  Infrared Nebula. Both stars fall on the same ISOPHOT pixel, and we provide
11  an upper limit to their combined fluxes.
12 Contaminated with flux from nearby PSC 11072-7727, the Infrared Nebula.
13 This source appears to be dramatically variable. While Prusti, Whittet, &
13  Wesselius (1992MNRAS.254..361P) give near-IR magnitudes, it went undetected
13  by the recent DENIS observations (Cambresy et al., 1998A&A...338..977C).
14 Contaminated with flux from nearby HD 97300.
15 IRAS FSC has a 12{mu}m measurement that is much too high to be photosphere,
15  though there is no indication that this has ever been identified as an IR
15  excess source. Our own observations with the UCLA double-beam infrared
15  camera at the Lick 3m Shane telescope show normal magnitudes at J and K
15  bands for this star's spectral type.
16 The SB nature of this source is unconfirmed. Odenkirchen et al.
16  (1998NewA....3..583O) note that the Hipparcos distance for this object is
16  inconsistent with its photometric distance and placing the star at the
16  cluster distance gives values for its space motion that are more consistent
16  with cluster mean values.
17 Once considered an Ursa Major candidate. Please see text.