S E A R C H E S F O R B R I G H T - R I M M E D C L O U D S W I T H I R A S

P O I N T S O U R C E S

K. SUGITANI College of General Education, Nagoya City University, Mizuho-ku, Nagoya 467, Japan

and

K. OGURA Kokugakuin University, Higashi, Shibuya-ku, Tokyo 150, Japan

Abstract. We have carried out systematic surveys for small bright-rimmed clouds asso- ciated with IRAS point sources in/around HII regions. They are candidate sites for star formation due to radiation-driven implosion.

Key words: Star Formation - - IRAS point sources - - HII Regions - - Radiation-driven Implosion --catalogs

Bright-r immed clouds are often found in /a round relatively old HII regions and have been suspected to be potential sites of star formation due to the compression by converging ionization-shock fronts. They are considered to be originally dense cores of the parental molecular clouds and have emerged after the dispersion of the ambient gas due to UV radiation from OB stars. Their physical conditions match well the theoretical models of radiation- driven implosion (e.g. Bertoldi 1989) and, therefore, induced star formation is generally expected there. We have systematically searched for small bright- r immed clouds associated with IRAS point sources to locate candidates for such star formation. The POSS atlas has been used in the northern sky, and the ESO(R) /SERC(J ) atlases in the southern sky.

Eighty-nine bright-r immed clouds associated with IRAS point sources have been selected (Table I). At least 19 (20 %) of the 89 clouds are known to be associated with molecular outflows, and six with HH objects. Most of their sizes are <1pc, and the luminosities of the associated IRAS point sources,

10 to 3 x 104L®, are much larger than those of the IRAS sources associated with Bok globules or dense cores in dark cloud complexes, both having a similar cloud mass range. This suggests that intermediate-mass stars or multiple star systems are mainly formed in the bright-r immed clouds. Also, IRAS luminosity to cloud mass ratios are significantly greater titan those in Bok globules or dense cores. The details are reported in Sugitani et al. (1991) and Sugitani & Ogura (1994)

Astrophysics and Space Science 224: 571-572, 1995. © 1995 Kluwer Academic Publishers. Printed in Belgium.

572 K. SUGITANI, K. OGURA

TABLE I

Bright-Rimmed Clouds Associated with IRAS Point Sources

IRAS IIH/ If%AS HH/

# H I I l ~ e g c~(1950) 6 ( 1 9 5 0 ) source flow # H I I l ~ e g c~(1950) 6 ( 1 9 5 0 ) s o u r c e f l o w

1 SlTl 23 56 53.3 67 06 57 23568+6706 45 RCWI4

2 S171 0 01 23.0 68 17 59 00013+6817 46 Gum Neb.

3 $171 0 02 47.9 67 00 57 00027+6700 47 S306

4 S 1 8 5 0 56 0 0 . 7 60 37 21 0 0 5 6 0 + 6 0 3 7 48 G u m N e b .

5 S 1 9 0 2 25 14 .5 61 20 10 0 2 2 5 2 + 6 1 2 0 I C 1 8 0 5 W 49 $ 3 0 7

6 S 1 9 0 2 30 5 7 . 7 60 34 41 0 2 3 0 9 + 6 0 3 4 50 G u m N e b .

7 $ 1 9 0 2 31 0 1 . 7 61 33 40 0 2 3 1 0 + 6 1 3 3 o u t f l o w 1 51 G u m N e b .

8 $ 1 9 0 2 31 48 ,1 61 06 32 0 2 3 1 8 + 6 1 0 6 52 G u m N e b .

9 $ 1 9 0 2 32 3 7 . 3 61 10 34 0 2 3 2 6 + 6 1 1 0 53 G u m N e b .

10 S 1 9 9 2 44 2 3 , 9 60 12 06 0 2 4 4 3 + 6 0 1 2 54 N G C 2 6 2 6

11 S 1 9 9 2 47 37 .4 59 50 54 0 2 4 7 6 + 5 9 5 0 55 R C W 2 7

12 S 1 9 9 2 51 0 8 . 3 60 23 35 0 2 5 1 1 + 6 0 2 3 o u t f l o w 1 56 R C W 2 7

13 S 1 9 9 2 57 0 3 . 6 60 28 29 0 2 5 7 0 + 6 0 2 8 o u t f l o w I 57 R C W 3 2

14 $ 1 9 9 2 57 3 5 . 6 60 17 22 0 2 5 7 5 + 6 0 1 7 G L 4 0 2 9 58 R C W 3 2

15 S 2 3 6 5 20 13 .3 33 09 08 0 5 2 0 2 + 3 3 0 9 59 I % C W 3 8

16 S 2 7 6 5 17 2 1 . 9 -5 55 05 0 5 1 7 3 . 0 5 5 5 R N O 4 0 60 I:{,CW38

17 $ 2 6 4 5 28 40 .2 12 03 13 0 5 2 8 6 + 1 2 0 3 61 N G C 3 5 0 3

18 $ 2 6 4 5 41 4 5 , 3 9 07 40 0 5 4 1 7 + 0 9 0 7 B 3 5 62 N G C 3 5 0 3

19 S 2 7 7 5 32 0 0 . 4 -3 00 12 0 5 3 2 0 - 0 3 0 0 o u t f l o w 1 63 N G C 3 5 0 3

20 S 2 7 7 5 35 33 ,2 -1 46 50 0 5 3 5 5 - 0 1 4 6 O r i - I 2 64 B B W 3 4 7

21 S 2 7 7 5 37 11 .8 -3 38 46 0 5 8 7 1 - 0 3 3 8 65 R C W 6 2

22 $ 2 8 1 5 35 5 8 . 5 -5 15 48 0 5 3 5 9 - 0 5 1 5 66 R C W 6 2

23 S 2 4 9 6 19 5 6 . 5 23 ii 32 0 6 1 9 9 + 2 3 1 1 67 R C W 6 2

24 $ 2 7 5 6 32 16 .5 4 2 7 40 0 6 3 2 2 + 0 4 2 7 68 R C W 6 2

25 $ 2 7 3 6 38 17 ,6 10 17 54 0 6 3 8 2 + 1 0 1 7 124 69 R C W 6 2

26 S 2 9 6 7 01 2 6 . 8 -11 41 17 0 7 0 1 4 - 1 1 4 1 70 I ~ C W 6 2

2 7 S 2 9 6 7 01 3 7 . 9 -11 18 48 0 7 0 1 6 - 1 1 1 8 71 ( C e n R 1 )

28 $ 2 9 6 7 02 2 1 . 4 - 1 0 17 25 0 7 0 2 3 - 1 0 1 7 72 1 ~ C W 7 5

29 $296 7 02 32.5 -12 04 51 07025-1204 73 RCW75

30 $ 49 18 15 5 5 . 0 -13 46 09 1 8 1 5 9 - 1 3 4 6 74 R C W 8 5

31 S l 1 7 20 48 57 .5 44 10 43 2 0 4 8 9 + 4 4 1 0 75 R C W 9 8

32 S131 21 30 5 2 . 7 57 I0 49 21308+5710 76 RCWI05

33 S 1 3 1 21 31 41 .1 57 16 13 2 1 3 1 6 + 5 7 1 6 77 (or S c o )

34 S131 21 32 0 2 , 5 57 50 06 2 1 3 2 0 + 5 7 5 0 o u t f l o w 1 78 (~ S c o )

35 S 1 3 1 21 34 3 5 . 8 58 18 1O 2 1 3 4 5 + 5 8 1 8 79 R C W 1 0 8

36 S131 21 34 40.1 57 14 05 21346+5714 80 RCWI08

37 S 1 3 1 21 38 5 3 . 2 56 22 18 2 1 3 8 8 + 5 6 2 2 G N 2 1 . 3 8 . 9 81 I ~ C W 1 0 8

38 S131 21 39 10.3 58 02 29 21391+5802 IC1396N 82

39 S131 21 44 30.8 57 12 29 21445+5712 IC1396E 83

40 S131 21 44 38.0 56 55 05 21446+5655 84

41 S131 21 44 52.8 57 04 46 21448+5704 85

42 S131 21 45 00.I 56 58 30 21450+5658 86

43 S142 22 45 48.5 57 46 59 22458+5746 87

44 8145 22 27 12.2 63 58 21 22272+6358A L1206 88

89

7 16 15 .5 -22 00 41 0 7 1 6 2 - 2 2 0 0

7 17 5 4 . 0 -44 29 24 0 7 1 7 8 - 4 4 2 9

7 29 3 6 . 9 -19 21 07 0 7 2 9 6 - 1 9 2 1

7 32 5 6 . 6 - 4 6 47 34 0 7 3 2 9 - 4 6 4 7

7 33 28 .0 -18 42 17 0 7 3 3 4 - 1 8 4 2

7 38 51 .4 -42 59 18 0 7 3 8 8 - 4 2 5 9

8 07 40 ,2 -35 56 07 0 8 0 7 6 - 3 5 5 6 120

8 24 16 .5 -50 50 44 0 8 2 4 2 - 5 0 5 0 4 6 / 4 7

8 25 0 3 . 4 -50 30 34 0 8 2 5 0 - 5 0 3 0

8 33 4 2 . 6 -40 28 02 0 8 3 3 7 - 4 0 2 8 1 3 5 / 6

8 39 2 3 . 4 -40 41 18 0 8 3 9 3 - 4 0 4 1

8 41 0 8 . 3 -39 49 05 0 8 4 1 1 - 3 9 4 9

8 42 18 .2 -41 05 19 0 8 4 2 3 - 4 1 0 5

8 43 35.7 -41 05 03 08435-4105

8 56 22.3 -47 II 17 08563-4711

8 58 19.1 -47 19 51 08583-4719

10 58 09.5-59 20 02 10581-5920

10 59 11.6 -59 34 52 10591-5934

11 01 13.5-59 31 50 II012-5931

11 10 07.4 -58 29 60 11101-5829

i i 30 37.9 -63 II 24 I1306-6311

11 31 31.4 -62 59 45 i1315-6259

I i 31 42.5 - 6 2 54 43 11317-6254

11 33 12.9 -62 58 15 11332-6258

11 38 49.0 -63 06 34 11388-6306

11 39 48.3 ~62 51 11 11398-6251

13 05 02.8 -61 54 26 13050-6154

13 15 51.5 -62 17 58 13158-6217

13 16 49.3 -62 08 19 13168-6208

14 15 59.2 -61 ii 30 14159-6111

15 51 56 .5 -54 30 14 1 5 5 1 9 - 5 4 3 0

16 06 5 6 . 7 -48 58 04 1 6 0 6 9 - 4 8 5 8

16 16 5 1 . 3 -25 26 29 1 6 1 6 8 - 2 5 2 6

16 17 5 0 . 8 - 2 5 01 Ol 16178-2501

16 36 14 .8 -48 45 54 1 6 3 6 2 - 4 6 4 5

16 36 31.8 -48 36 35 16365-4836

16 37 22 ,2 -49 i i 59 1 6 3 7 3 - 4 9 1 1

I ~ C W l 1 3 / 6 16 43 2 1 . 0 -41 08 32 1 6 4 3 8 - 4 1 1 0

B ~ C W l l 3 / 6 16 48 4 3 . 2 -40 43 09 1 6 4 8 7 - 4 0 4 3

RCWII3/6 16 50 17.5 -40 02 29 16502-4002

R C W l l S / 6 16 55 33 .3 -42 37 33 1 6 5 5 5 - 4 2 3 7

R C W 1 3 4 17 46 2 1 . 5 -31 28 20 1 7 4 6 3 - 3 1 2 8

M 8 17 59 47 .5 -24 22 14 1 7 5 9 7 - 2 4 2 2

M8 18 01 13.i -24 07 11 18012-2407

S i m e i s 188 18 06 5 0 . 7 - 2 4 05 33 1 8 0 6 8 - 2 4 0 5

1Sugitani L: Ogura (1994)

R e f e r e n c e s

Bertoldi 1989, ApJ, 346, 735 Sugitani et al. 1991, ApJS, 77, 59 Sugitani ~z Ogura 1994, ApJS, 92, 163