A&A 380, 609-614 (2001)
DOI: 10.1051/0004-6361:20011476

A photometric catalogue of southern emission-line stars[*],[*]

D. de Winter1,2,3 - M. E. van den Ancker4 - A. Maira1 - P. S. Thé5 - H. R. E. Tjin A Djie5 - I. Redondo1 - C. Eiroa1 - F. J. Molster5,6


1 - Dpto. Física Teórica, C-XI, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain
2 - Instituto de Astrofísica de Canarias, C/ Via Láctea s/n, 38200 La Laguna, Tenerife, Spain
3 - TNO TPD, Stieltjesweg 1, PO Box 155, 2600 AD Delft, The Netherlands
4 - Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, MS 78, Cambridge, MA 02138, USA
5 - Astronomical Institute, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands
6 - School of Materials Science and Engineering, Georgia Tech, Atlanta, GA 30332-0245, USA

Received 19 June 2001 / Accepted 18 October 2001

Abstract
We present a catalogue of previously unpublished optical and infrared photometry for a sample of 162 emission-line objects and shell stars visible from the southern hemisphere. The data were obtained between 1978 and 1997 in the Walraven (WULBV), Johnson/Cousins ( $UBV(RI)\rm _c$) and ESO and SAAO near-infrared (JHKLM) photometric systems. Most of the observed objects are Herbig Ae/Be (HAeBe) stars or HAeBe candidates appearing in the list of HAeBe candidates of Thé et al. (1994), although several B[e] stars, LBVs and T Tauri stars are also included in our sample. For many of the stars the data presented here are the first photo-electric measurements in the literature. The resulting catalogue consists of 1809 photometric measurements. Optical variability was detected in 66 out of the 116 sources that were observed more than once. 15 out of the 50 stars observed multiple times in the infrared showed variability at 2.2 $\mu$m (K band).

Key words: circumstellar matter - stars: emission-line - stars: pre-main sequence - infrared: stars


1 Introduction

One of the classic characteristics of a young star is the presence of photometric variability. Several types of photometric variability can be recognized, amongst which are more or less periodic variability due to magnetic activity on the stellar surface (star spots), brightness variations due to a variable rate of accretion, and irregular large-amplitude (>0 $.\!\!^{\rm m}$5) variations due to variable circumstellar extinction (Bibo & Thé 1991; Shevchenko et al. 1993; Herbst et al. 1994; van den Ancker et al. 1998; Herbst & Shevchenko 1999). However, a detailed analysis of a star's photometric behaviour requires great amounts of data, preferably over a large period of time. In practice, sufficient data can often only be obtained by combining data sets from the literature with new data.

Herbig Ae/Be (HAeBe) stars may be one of the most interesting groups of young stars to study since they are intrinsically bright and therefore can be seen over great distances, tracing galactic regions of star formation. Furthermore, many are sufficiently bright to be observed with smaller telescopes, allowing detailed studies of their photometric behaviour to be made. A catalogue of 287 candidate members of the Herbig Ae/Be stellar group was published by Thé et al. (1994). For many of the objects in this catalogue little or no data is available and therefore a new investigation of their properties is in order.

In this paper we present photometry of 162 emission-line and shell stars, most of which appear in the list of HAeBe candidates by Thé et al. Names, positions and classifications of the stars are listed in Table 1. Section 2 gives a detailed description of the observations. Although a brief discussion of the data is presented in Sect. 3, we defer a detailed analysis of these data to future papers in which these data can be combined with photometry over a much longer time span.

 
Table 1: Properties of programme stars.

Name		 Cat. Des. Other $\alpha$ (2000) $\delta$ (2000) Type # Observations $V_{\rm obs}$ $V_{\rm lit}$ Ref.
 

       $^{\rm h}$   $^{\rm m}$   $^{\rm s}$     $^{\circ}$   '   ''   WULBV UBVRI JHKLM [mag] [mag]  

71 Cet		 HD 15004   02 24 58.4 -02 46 48 A-sh  2 - - 6.34-6.65 6.31-6.36 (1)
BU Tau HD 23862 MWC 75 03 49 11.2 +24 08 12 Be  1 - - 5.08 5.01-5.07 (1)
V1080 Tau HD 283817 StH$\alpha$ 33 04 40 32.6 +24 26 31 HAe  2  3 - 10.10-11.68 10.29-10.56 (2)
AB Aur HD 31293 MWC 93 04 55 45.8 +30 33 04 HAe  1  2 - 7.02-7.04 7.03-7.13 (1)
  HD 31648 MWC 480 04 58 46.3 +29 50 37 HAe  2  3 - 7.68-7.72 7.66-7.86 (1)
UX Ori HD 293782   05 04 30.0 -03 47 14 HAe 29 13 12 9.84-11.79 9.66-11.79 (3)
V1012 Ori     05 11 36.4 -02 22 47 HAe -  6 - 12.07-13.12 12.5-16.5pg (2)
S22/LMC HD 34664 MWC 105 05 13 53.1 -67 26 54 B[e] -  3 - 11.77-12.65    
V1366 Ori HD 34282   05 16 00.5 -09 48 35 HAe -  3 - 9.81-9.94    
V346 Ori HD 287841   05 24 42.8 +01 43 48 HAe 22  6  3 10.09-10.84 10.17-10.38 (3)
CO Ori BD+11 809   05 27 38.3 +11 25 39 HFe -  3 - 11.25-11.70 9.81-12.52 (4)
  HD 35929   05 27 42.8 -08 19 38 HFe -  5  1 8.11-8.31    
Par 102 BD-06 1193 StH$\alpha$ 41 05 29 11.4 -06 08 05 HFe -  8  3 10.43-10.54    
  BD+11 820   05 29 22.1 +11 50 50 HAe? -  1 - 10.84    
  HD 36112 MWC 758 05 30 27.5 +25 19 57 HAe -  2 - 8.26-8.27 8.20-8.44 (1)
HK Ori   MWC 497 05 31 28.0 +12 09 11 HFe 23  5  3 11.41-11.67 11.39-12.10 (4)
  HD 244604   05 31 57.3 +11 17 41 HAe -  3 - 8.99-9.38 9.18-9.71 (1)
RY Ori     05 32 10.0 -02 49 49 HFe  8  4  3 11.57-12.68 11.08-12.96 (3)
EZ Ori   Par 1409 05 34 18.6 -05 04 48 TT -  1 - 12.87 12.0-14.1pg (2)
IX Ori   Par 1552 05 34 40.8 -05 22 43 TT -  4  1 12.33-13.26 13.4-15.5pg (2)
V372 Ori HD 36917 Par 1605 05 34 47.0 -05 34 15 A-sh 10  3  3 7.98-8.00 7.98-8.03 (3)
YZ Ori   Par 1648 05 34 54: -05 03 30: TT -  4  1 13.74-14.85 13.9-16.6pg (2)
Par 1660 HD 36939   05 34 55.3 -05 30 22 HBe?  9  3  3 8.97-9.00 8.98-9.02 (3)
Par 1623 BD-05 1306   05 34 55.6 -05 16 43 A-sh 10  2  2 10.13-10.19    
KS Ori   Par 1685 05 35 00.1 -05 25 16 A-sh 10  2  1 10.05-10.12 9.7-12.0pg (2)
V1271 Ori HD 245185   05 35 09.6 +10 01 52 HAe -  6 - 9.91-9.98 9.85-9.95 (3)
MR Ori     05 35 17.0 -05 21 46 A-sh -  3 - 9.54-10.85 10.3-12.0 (2)
LZ Ori HD 294263 Par 1854 05 35 17.8 -04 41 07 A-sh 20  1  3 9.73-10.09 10.3-11.1pg (2)
MX Ori BD-05 1317 Par 1953 05 35 21.3 -05 09 16 HFe -  1 - 9.31 10.3-11.7pg (2)
NV Ori BD-05 1324 Par 2086 05 35 31.3 -05 33 09 HFe  6 -  2 9.63-9.90 9.78-10.35 (3)
V361 Ori HD 37062 Par 2085 05 35 31.4 -05 25 16 B-sh  9  1  3 8.15-8.20 8.14-8.24 (3)
T Ori BD-05 1329 MWC 763 05 35 50.4 -05 28 35 HAe 25 10  7 10.15-11.04 10.00-11.95 (3)
CQ Tau HD 36910   05 35 58.5 +24 44 54 HFe  1  4 - 10.22-11.06 9.36-11.14 (3)
V380 Ori BD-06 1253 MWC 765 05 36 25.4 -06 42 58 HAe 25 12  7 10.21-10.73 9.46-11.22 (4)
BN Ori HD 245465   05 36 29.3 +06 50 02 A-sh 11  3  2 9.62-9.68 9.56-9.71 (5)
Par 2441 BD-04 1191   05 36 51.2 -04 25 40 TT -  1 - 10.74    
V586 Ori HD 37258 Par 2473 05 36 59.3 -06 09 16 HAe 24  8  3 9.64-10.08 9.53-10.77 (3)
BF Ori BD-06 1259   05 37 13.3 -06 35 01 HAe 25 14  9 9.82-11.67 9.59-11.92 (3)
Par 2599 HD 37357 KMS 27 05 37 47.1 -06 42 30 HAe -  7  2 8.83-8.84 8.83-8.91 (4)
N3Sk81   KMS 34 05 38 08.8 -06 49 13 HAe -  6  1 13.75-13.84    
Par 2653 HD 37411   05 38 14.5 -05 25 13 HAe  2 10  1 9.76-9.85 9.79-9.81 (4)
  CD-59 1105   05 38 33.0 -59 04 28 Fe -  1 - 9.74    
N3Sk83 =V883 Ori? KMS 40 05 38 18.1 -07 02 26 HBe -  1  1 14.4    
V599 Ori   KMS 49 05 38 54.4 -07 16 38 HAe -  2  1 13.76-13.80 15.1-16.3pg (2)
$\omega$ Ori HD 37490 MWC 117 05 39 11.1 +04 07 17 Be -  3 - 4.48-4.56 4.49-4.55 (1)
V350 Ori     05 40 11.6 -09 42 10 HAe  4 16  3 10.77-13.32 10.71-13.24 (3)
KMS 82     05 40 37.2 -08 04 02: HFe? -  4  2 11.55-14.57    
KMS 108     05 40 46.3 -08 53 48: HBe? -  2  1 11.19-11.21    
  HD 37806 MWC 120 05 41 02.3 -02 43 01 HAe  9  7  2 7.86-7.96 7.89-7.98 (3)
KMS 118     05 41 03.9 -09 23 18: HFe -  3  1 14.80-14.92    
V351 Ori HD 38238   05 44 18.8 +00 08 40 HAe  8  2  4 8.89-9.13 8.81-10.94 (6)
FU Ori BD+09 5427 CDS 535 05 45 22.4 +09 04 12 FUOR  2  1 - 9.09-9.32 8.02-10.06 (4)
  HD 288313   05 54 03.0 +01 40 22 TT -  7 - 9.45-9.95    
V1307 Ori HD 250550 MWC 789 06 02 00.0 +16 30 57 HBe 14 -  2 9.53-9.56 9.54-9.88 (3)
17 Lep HD 41511 MWC 519 06 04 59.1 -16 29 04 A-sh  2  3 - 4.91-5.01 4.97-5.02 (1)
LkH$\alpha$ 208     06 07 49.4 +18 39 27 HAe -  3 - 11.04-11.50 11.36-12.21 (4)
LkH$\alpha$ 339     06 10 54.4 -06 14 39 HAe -  5  1 13.44-13.64 13.65-13.67 (4)



 
Table 1: continued.

Name		 Cat. Des. Other $\alpha$ (2000) $\delta$ (2000) Type # Observations $V_{\rm obs}$ $V_{\rm lit}$ Ref.
 

       $^{\rm h}$   $^{\rm m}$   $^{\rm s}$     $^{\circ}$   '   ''   WULBV UBVRI JHKLM [mag] [mag]  

V1308 Ori		   MWC 137 06 18 45.5 +15 16 52 HBe -  2 - 11.67-11.98 11.79-12.27 (4)
FS CMa HD 45677 MWC 142 06 28 17.4 -13 03 11 B[e] 17 13  2 7.94-8.74 7.22-8.85 (7)
VY Mon     06 31 06.9 +10 26 05 HBe -  3 - 12.97-13.09 12.77-14.77 (4)
V699 Mon   LkH$\alpha$ 215 06 32 41.8 +10 09 34 HBe 19  5  2 10.46-10.91 10.36-10.84 (2)
V700 Mon HD 259431 MWC 147 06 33 05.2 +10 19 20 HBe 13  6  2 8.69-8.75 8.65-8.97 (1)
R Mon BD+08 1427 MWC 151 06 39 09.9 +08 44 10 HBe 13  4  2 10.35-12.41 11.60-12.54 (4)
V590 Mon W90 LkH$\alpha$ 25 06 40 44.6 +09 48 02 HFe -  8  1 11.88-12.94 12.60-12.95 (4)
ST Pup CD-37 3101   06 48 56.4 -37 16 33 Ceph. -  1 - 10.31 9.28-10.68 (2)
V743 Mon HD 50138 MWC 158 06 51 33.4 -06 57 59 B[e] 20 13  2 6.59-6.85 6.53-6.65 (1)
GU CMa HD 52721 MWC 164 07 01 49.5 -11 18 03 HBe  1  2 - 6.50-6.57 6.52-6.71 (1)
Z CMa HD 53179 MWC 165 07 03 43.2 -11 33 06 FUOR 19 19  6 8.68-10.27 8.61-10.22 (4)
HU CMa   LkH$\alpha$ 220 07 04 06.8 -11 26 07 HBe -  3 - 11.52-11.92 11.57-12.19 (4)
V750 Mon HD 53367 MWC 166 07 04 25.5 -10 27 16 HBe 12  4  3 6.92-7.08 7.00-7.22 (1)
NX Pup CD-44 3318 Hen 3-32 07 19 28.3 -44 35 11 HAe 15  7  3 9.63-11.08 9.53-10.99 (3)
V694 Mon   MWC 560 07 25 51.3 -07 44 08 Symb. -  8 - 9.96-10.33 9.10-10.10 (2)
  HD 58647   07 25 56.1 -14 10 44 A-sh - -  1   6.76-6.88 (1)
  HD 59319 MWC 843 07 28 36.8 -21 57 49 HBe? -  4 - 8.29-8.31 8.19-8.47 (1)
  HD 59771   07 30 51.1 -18 15 43 Fe -  2 - 8.89-8.94 8.83-9.31 (1)
Hen 3-40   Wray 15-30 07 31 48: -41 34 00: Ge -  3  1 13.73-14.42    
PW Pup CD-30 5135 Hen 3-83 07 49 06.0 -31 07 43 Fe -  2 - 9.23-9.24 9.27-9.97 (1)
V402 Pup HD 64315   07 52 20.3 -26 25 47 Oe -  1 - 9.24 8.99-9.39 (1)
AS 202 CD-37 4833 Hen 3-174 08 32 35.8 -37 59 02 HBe? -  1 - 10.80 9.70-10.70 (2)
ESO 313-10     08 42 17.0 -40 44 13: HBe -  3  1 14.24-14.59    
Hen 3-209   Wra 15-285 08 48 45.5 -46 05 08 B[e] -  1 - 13.56    
Hen 2-14   Wra 16-30 08 51 59.5 -46 18 05: B[e] -  1 - 14.05    
OU Vel HD 76534 Hen 3-225 08 55 08.7 -43 28 00 HBe  2  2  2 7.96-8.08    
RCW 34   Gum 19 08 56 27.8 -43 05 46: O -  2 - 11.21-11.64    
Herbst 28   Bran 215 08 58 26.3 -43 26 10 Be -  2  1 11.25-14.76    
RCW 36   Bran 217 08 59 00.9 -43 44 10 HFe? -  1 - 15.20    
  HD 309784 Hen 3-315 09 42 36.4 -67 08 54 B[e] -  1 - 10.16    
  HD 85567 Hen 3-331 09 50 28.5 -60 58 03 HBe - 33 - 8.49-8.59 8.44-8.75 (1)
  HD 87643 MWC 198 10 04 30.3 -58 39 52 B[e] 22 16  3 8.52-9.00 8.68-9.20 (3)
17 Sex HD 88195   10 10 07.5 -08 24 29 B-sh  1 - - 5.90 5.87-5.93 (1)
  HD 89249 MWC 200 10 16 20.6 -55 35 51 Be -  1  1 8.90 8.70-9.15 (1)
HR Car HD 90177 MWC 202 10 22 53.8 -59 37 28 LBV 21 11  3 7.44-8.42 7.40-8.34 (3)
Hen 3-416   Th 35-40 10 25 44.5 -58 33 52 HBe? -  1 - 10.59    
Wra 15-566     10 25 51.7 -60 53 14 TT? -  2 - 13.87-13.90    
V503 Car HD 90578 Hen 3-418 10 26 00.2 -57 49 37 B[e] -  1 - 9.33 9.08-9.75 (1)
  HD 92061 Hen 3-455 10 36 24.2 -58 57 09 HBe? -  1 - 8.97 8.99-9.87 (1)
  CPD-59 2617 Hen 3-480 10 44 49.4 -59 49 28: HBe? - -  1      
  HD 94509 Hen 3-515 10 53 27.3 -58 25 25 HBe -  4 - 9.08-9.13 8.85-9.41 (1)
  CPD-59 2854 Wra 15-689 10 55 55.4 -60 14 20 B[e] -  1 - 10.54    
GG Car HD 94878 MWC 215 10 55 58.9 -60 23 33 B[e] 23 14  3 8.53-9.03 8.48-9.00 (8)
  HD 305773 CD-59 3426 10 56 03.9 -60 29 38 HBe? -  1 - 9.08 8.80-9.39 (1)
AG Car HD 94910 MWC 216 10 56 11.6 -60 27 13 LBV 22 11  3 6.49-7.00 6.10-8.12 (9)
HR 4329 HD 96706   11 06 49.9 -70 52 41 B-sh  2 - - 5.58-5.59 5.54-5.60 (1)
DI Cha CD-76 486 Hen 3-593 11 07 20.7 -77 38 07 TT 23  3  3 10.65-10.74 10.66-10.74 (10)
CU Cha HD 97048 Hen 3-597 11 08 03.3 -77 39 17 HAe 23  9  7 8.40-8.48 8.44-8.48 (10)
  HD 97240   11 09 18.1 -77 47 40 F-sh  2 - - 8.49-8.50 8.42-8.69 (1)
  HD 97300   11 09 50.0 -76 36 48 B-sh -  4  1 9.02-9.08 8.97-9.03 (1)
  HD 98922 Hen 3-644 11 22 31.7 -53 22 11 HBe  2 38 - 6.72-6.81 6.72-6.83 (1)
KR Mus HD 100546 Hen 3-672 11 33 25.4 -70 11 41 HBe  2  4  1 6.69-6.74 6.71-6.77 (3)
  HD 101412 Hen 3-692 11 39 44.5 -60 10 28 HBe -  6  1 9.24-9.28 8.97-9.56 (1)
V644 Cen HD 306989 Hen 3-700 11 43 06.5 -60 44 05 Be -  1  1 10.52 9.91-10.33 (10)
DX Cha HD 104237 Hen 3-741 12 00 05.1 -78 11 35 HAe  2 38  1 6.49-6.59 6.56-6.68 (1)
  HD 105234   12 07 05.5 -78 44 28 A-sh  2 - - 7.48-7.48 7.45-7.59 (1)
RU Cen HD 105578 Hen 3-755 12 09 23.8 -45 25 35 Ge -  1 - 8.63 8.78-9.56 (1)



 
Table 1: continued.

Name		 Cat. Des. Other $\alpha$ (2000) $\delta$ (2000) Type # Observations $V_{\rm obs}$ $V_{\rm lit}$ Ref.
 

       $^{\rm h}$   $^{\rm m}$   $^{\rm s}$     $^{\circ}$   '   ''   WULBV UBVRI JHKLM [mag] [mag]  

Hen 3-759		     12 12 08.6 -62 29 01 Be -  1 - 10.47    
DK Cha IRAS12496-7650   12 53 16.1 -77 07 02: HAe - -  1      
V1028 Cen CD-48 7859 Hen 3-847 13 01 17.8 -48 53 19 HAe - 34  2 10.56-10.65    
LSS 3027B CPD-61 3587B   13 19 04.0 -62 34 10 HBe  1  2  3 15.17-15.24    
CQ Cir HD 130437 Hen 3-1031 14 50 50.3 -60 17 10 HBe -  7  1 9.85-9.91    
SS73 44     15 03 23.9 -63 22 54 HBe -  2  1 14.75-16.80    
  HD 132947   15 04 56.1 -63 07 53 HAe -  1 - 8.91 8.73-9.12 (1)
HT Lup CD-33 10685 Hen 3-1095 15 45 12.9 -34 17 31 TT  9 - - 10.21-10.26 10.26-10.40 (2)
  HD 140817   15 47 04.5 -35 30 37 B-sh  2 - - 6.83-6.84 6.77-6.90 (1)
  HD 141569   15 49 57.7 -03 55 16 HAe -  1 - 7.10 7.11-7.14 (3)
  HD 144432 Hen 3-1141 16 06 58.0 -27 43 10 HAe -  1 - 8.17 8.08-8.35 (1)
V856 Sco HD 144668 HR 5999 16 08 34.3 -39 06 18 HAe  9 26 13 6.55-7.32 6.64-7.95 (3)
V1027 Sco HD 144667 HR 6000 16 08 34.6 -39 05 34 B-sh  7  8  9 6.65-6.73 6.65-6.67 (3)
  HD 147196   16 21 19.2 -23 42 29 Be -  5  2 7.00-7.04 7.02-7.12 (1)
Wra 15-1484   Hen 3-1191 16 27 14.2 -48 39 28 B[e] - 44 - 12.52-13.91    
V2307 Oph HD 150193 MWC 863 16 40 17.9 -23 53 45 HAe  3 11  1 8.80-8.88 8.79-8.87 (10)
AK Sco HD 152404   16 54 44.8 -36 53 19 HFe  3  5  2 8.81-9.18 8.76-9.93 (3)
AS 215 HD 322422 Hen 3-1293 16 57 23.9 -40 21 40 B[e] -  6 - 9.68-9.71 9.71-9.75 (3)
V921 Sco CD-42 11721 MWC 865 16 59 06.9 -42 42 08 B[e]  4  7  4 11.10-11.36 11.43-11.73 (2)
V1104 Sco HD 326823 Hen 3-1330 17 06 53.9 -42 36 40 B[e] -  8 - 8.98-9.04 8.90-9.33 (1)
KK Oph   Hen 3-1346 17 10 08.1 -27 15 18 HAe  3  7  1 11.32-12.36 11.37-11.87 (3)
Wra 15-1651     17 14 45.6 -36 18 35: HBe? - -  1      
Wra 15-1678     17 20 14.8 -37 39 35: HBe? - -  1      
  HD 156702 MWC 257 17 20 50.6 -38 39 09 B[e] -  4 - 8.70-8.72 8.58-8.83 (1)
51 Oph HD 158643 HR 6519 17 31 25.0 -23 57 46 Be  2  7 - 4.77-4.81 4.77-4.82 (1)
XX Oph HD 161114 MWC 269 17 43 56.5 -06 16 09 Symb. 11  5  1 8.80-9.08 8.80-9.11 (3)
  HD 163296 MWC 275 17 56 21.3 -21 57 22 HAe  8 15  4 6.82-6.93 6.82-6.93 (1)
LkH$\alpha$ 108     18 03 50.6 -24 21 11 HBe?  2 - - 11.67-11.71    
V4203 Sgr CD-24 13830 LkH$\alpha$ 112 18 04 22.5 -24 22 10 HBe  2  2  1 9.95-9.98 9.54-10.19 (4)
  HD 164906 MWC 280 18 04 25.8 -24 23 08 Oe  3  2 - 7.46-7.49 7.32-7.59 (1)
LkH$\alpha$ 115     18 04 50.4 -24 25 42 HBe?  3  2  1 11.95-11.96 10.80-12.25 (4)
LkH$\alpha$ 118 CD-24 13874 Hen 3-1583 18 05 49.6 -24 15 20 Be  5  6  3 11.11-11.18 10.69-11.61 (4)
LkH$\alpha$ 119     18 05 56: -24 14 24: Be  5  6  3 12.15-12.21 11.27-12.76 (4)
NZ Ser   MWC 297 18 27 39.6 -03 49 52 HBe  6  5 - 12.03-12.63 11.95-12.60 (4)
VV Ser     18 28 47.9 +00 08 40 HAe  1  4 - 11.81-12.31 11.18-13.09 (4)
V431 Sct   MWC 300 18 29 25.7 -06 04 37 B[e]  1  1 - 11.73-11.79 11.54-11.90 (4)
AS 310   MH$\alpha$ 375-17 18 33 21.2 -04 58 07 HBe  1  1  4 12.47-12.59 12.08-13.19 (4)
HR 7169 HD 176269   19 01 03.2 -37 03 39 B-sh  2 - - 6.72-6.74 6.63-6.73 (1)
HR 7170 HD 176270   19 01 04.3 -37 03 42 B-sh  1 - - 6.45 6.34-6.44 (1)
S CrA   Hen 3-1731 19 01 20: -36 57 00: TT  8 - - 10.46-11.76 10.80-12.44 (4)
  HD 176386   19 01 38.9 -36 53 27 B-sh 11  6  3 7.27-7.43 7.27-7.30 (3)
TY CrA CD-37 13024   19 01 40.8 -36 52 34 A-sh 12  6  5 9.34-9.70 9.06-9.79 (3)
R CrA CD-37 13027 Hen 3-1733 19 01 53.7 -36 57 08 HAe  8 10  6 12.10-13.72 10.18-14.65 (4)
T CrA     19 01 58.8 -36 57 49 HFe  7  2  4 13.27-14.10 12.10-13.99 (4)
  HD 179218 MWC 614 19 11 11.3 +15 47 16 HBe  1 - - 7.39 7.34-7.47 (1)
WW Vul HD 344361 MWC 987 19 25 58.8 +21 12 31 HAe 10  8 - 10.48-11.68 10.25-12.40 (4)
V1295 Aql HD 190073 MWC 325 20 03 02.5 +05 44 17 HAe  1 - - 7.86 7.84-7.89 (10)
HR 7836 HD 195325 MWC 1019 20 30 18.0 +10 53 45 HBe?  2 - - 5.97-6.03 6.00-6.09 (1)

Total:		 162 stars         753  830  229       

Explanation of the abbreviations used: HAe/Be = Herbig Ae/Be star; HFe = F-type Herbig-like star; TT = T Tauri star; FUOR = FU Orionis type star; A-, B-sh: A- or B- type star with shell lines; Be = classical Be star; B[e] = B[e] star; Symb. = symbiotic star; Ceph. = Cepheid; LBV = Luminous Blue Variable.

References: (1) Tycho Catalogue (ESA 1997); (2) General Catalogue of Variable Stars (Kholopov et al. 1998); (3) ESO Long Term Photometry of Variables data (Manfroid et al. 1991, 1995; Sterken et al. 1993, 1995); (4) Herbst & Shevchenko (1999); (5) Shevchenko et al. (1997); (6) van den Ancker et al. (1996); (7) de Winter & van den Ancker (1997); (8) Gosset et al. (1984); (9) Sterken et al. (1996); (10) Kilkenny et al. (1985).


2 Observations

Photometric data in the Walraven WULBV system of our programme stars were obtained between 1978 and 1988 at the 90 cm Dutch Light Collector. The data taken in 1978 were obtained when this telescope was located in Hartebeespoortdam, South Africa. All observations in later years were obtained after the telescope had been moved to the European Southern Observatory, La Silla, Chile. A detailed description of the Walraven photometric system can be found in de Geus et al. (1989), who also explain the employed measuring and data reduction procedures. All data presented here were made with a 5-channel photometer which measures all Walraven WULBV intensities simultaneously, thereby avoiding any systematic effects due to non-simultaneous measurements at the different photometric passbands. A circular diaphragm with a diameter of 21 $.\!\!^{\prime\prime}$5 was used for all stars. Typical errors in the data, given in $\log_{10}$ intensity values, are 0.004, 0.003, 0.004, 0.006, and 0.009 for V, V-B, B-U, U-W, and B-L, respectively. Results of the photometric measurements in the Walraven system are listed in Table 2 (only available electronically at the CDS). The last column in this table lists the corresponding V magnitude in the Johnson photometric system, computed using the transformation formula by Brand & Wouterloot (1988). Also listed in Table 2 are the date and heliocentric Julian date (JD) of each observation. In some cases, the exact universal time of individual observations proved impossible to reconstruct. In those cases, only the integer fraction of the JD is listed.

Optical photometry in the Johnson/Cousins $UBV(RI)\rm _c$ system was obtained at La Silla with the ESO 50 cm and 1 m telescopes, during several observing runs between 1979 and 1994. Additional $UBV(RI)\rm _c$ photometry was obtained in February 1997 at the South African Astronomical Observatory (SAAO) using the SAAO 75 cm telescope. During these observations, mostly made through a 15 $^{\prime\prime}$ circular diaphragm, the telescope was equipped with a single channel photometer and either a Quantacon RCA 3103A (pre-1993) or EMI 9658RA (post-1993) photo-multiplier. The observations through U, B, V, $R\rm _c$ and $I\rm _c$ filters were made consecutively, in ascending or in descending order. Data were reduced with the Dutch method, using the E-region standard stars from the list by Graham (1982). Non-variable K and M0 standards were always included to avoid large transformation errors. Typical errors in the resulting data, listed in Table 3 (only available electronically at the CDS), are 0 $.\!\!^{\rm m}$01, 0 $.\!\!^{\rm m}$01, 0 $.\!\!^{\rm m}$02, 0 $.\!\!^{\rm m}$01, 0 $.\!\!^{\rm m}$02 for V, B-V, U-B, V-R and V-I, respectively. For stars fainter than 12th magnitude the errors may be twice those values. A colon following the data indicates that these particular data are more uncertain than the values listed here. Two colons indicates very uncertain data.

Near-IR photometric data in the ESO JHKLM system (Bouchet et al. 1989, 1991), of the programme stars were obtained with the ESO 1 m telescope at La Silla on several occasions between 1979 and 1995. Additional Near-IR observations in the SAAO JHKLM system (Carter 1990; Carter & Meadows 1995) were obtained with the 1.9 m telescope at the SAAO in 1997. During the near-IR observations, made through a 13 $^{\prime\prime}$ diaphragm, the telescope was equipped with a photovoltaic InSb detector unit. Standard stars were obtained from the list by Bouchet et al. (1991). Sky subtraction was achieved by chopping, with a frequency of 8 Hz, in the east-west direction with a throw of 30 $^{\prime\prime}$ amplitude. The J, H, K, L and M magnitudes were again measured consecutively, in ascending or in descending order. Typical errors in these data are 0 $.\!\!^{\rm m}$04, 0 $.\!\!^{\rm m}$04, 0 $.\!\!^{\rm m}$03, 0 $.\!\!^{\rm m}$05, 0 $.\!\!^{\rm m}$06 for the J, H, K, L and M magnitudes, respectively. The resulting near-IR magnitudes of our programme stars are listed in Table 4 (only available electronically at the CDS).

3 Discussion

A summary of all 1809 new photometric measurements is given in the last four columns of Table 1, which list the number of obtained measurements in the Walraven, Johnson/Cousins and Near-IR photometric systems, as well as the observed range in V magnitude. Note that for some stars with a small range in V, this is entirely compatible with the expected errors in our measurements. Also listed in Table 1 is the range of photometric values found in the literature. Ranges derived from photographic rather than photo-electric data are indicated by the suffix "pg''. In most cases the range observed by us is within the previously known range. In other cases (e.g. V1080 Tau), the data presented here expands the known variability range. In some objects (e.g. LkH$\alpha$ 339, V921 Sco) the range in V magnitude observed by us is completely out of the range known from literature. In those cases one might expect the star to show variations on time scales longer than those covered by our data.

Although a detailed analysis of all the data presented here is beyond the scope of this paper, we note that the statistical properties of the observed variations are in good agreement with previous work. Of the 116 stars with more than one measurement in Tables 2 or 3, 66 (or 57%) show variability in the V band with a magnitude exceeding 0 $.\!\!^{\rm m}$1. This is very close to the 65% of HAeBes showing significant variations in the study by van den Ancker et al. (1998). The slightly lower fraction found here can easily be explained by the smaller number of measurements per star in the current study, causing us to not detect variability in some known variables.

In the case of near-infrared variability, literature data is much more scarce (in fact, for many of the stars the data listed in Table 4 are the first JHKLM measurements in the literature). Therefore a comparison with previous work is more cumbersome. Of the 50 stars with more than one measurement in Table 4, 15 show significant (>0 $.\!\!^{\rm m}$2) variability in their K (2.2 $\mu$m) magnitude. Again we must caution that in view of the limited amount of measurements per star this will certainly be an underestimate of the number of near-infrared variables in our sample. In fact, in some cases the magnitudes we provide differ by more than 0 $.\!\!^{\rm m}$5 with determinations from the literature (Gezari et al. 1999; Eiroa et al. 2001). This could indicate variability of the circumstellar disk around these objects, rather than the variable circumstellar obscuration commonly associated with large-amplitude optical brightness variations. Consequently these stars are good candidates for further studies.

The data presented here are suitable to be combined with the photometric data of the studied stars already present in the literature to perform a more detailed analysis of the photometric behaviour of the stars in our sample. However, the main value of the catalogue presented here may be for historical reference. It is well known that some young stars with well-documented historical variability (e.g. AB Aur, BN Ori, V351 Ori) have in recent years displayed a constant brightness for decades or longer. It is likely that some stars in our sample which have remained relatively constant over the time-frame studied here will become more active in years to come and vice-versa, that our variable stars may at some time cease to vary. In those cases, the information presented in Tables 2-4 will be extremely valuable in exploring the presently unknown cause of such long-term changes in photometric behaviour of young stars.

Acknowledgements
The authors would like to thank the staff at ESO La Silla and at the SAAO for the excellent help during the various observing runs. We would also like to thank several persons who spent long nights observing some of the data listed in this paper, and were not mentioned before. In alphabetic order: S. van Amerongen, E. A. Bibo, H. Cuypers, A. Hollander, M. Janssens, Y. K. Ng, R. van Ojik, L. Remijn and J. M. Smit. We are also indebted to Dr. A. van Genderen for his many years of work into maintaining the Walraven photometry programme on the Dutch telescope at La Silla. The referee, C. Catala, provided many suggestions for improvements of the paper, for which we thank him. This research has made use of the Simbad data base, operated at CDS, Strasbourg, France.

References

 
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