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1989AJ.....97..786Hughes & MacLeod

The use of IRAS data to define HII regions

V.A. Hughes & G.C. McLeod

Abstract

Creteria derived optically identified objects have been used initially to identify infrared HII regions from the IRAS PSC, to a confidence level of 89%. By relaxing these creterias somewhat, it has been found possible ti increase the number to 2298 sources, at the confidence level of at least 77%. It is highly likely that the latter is greatly underestimated, since infrared HII regions are much stronger than confusing objects, and are thus seen to greater distances. A latitude-longitude plot shows that most of the HII regions lie, as expected, within +-3^o of the galactic plane, and also show some structure, in particular the local spiral arm. Also from 949 IRAS sources that are likely planetary nebulae to a 79% confinece level. The planetary nenulae have a much wider, +- 10^o, distribution about the plane. As a test of the anylysis, seven of the sources with high values of log (S_25/S_12) have been observed with the VLA. Six were detected as objects having an angular size of a few arcseconds.

see also 1994APJ...427..857-866Hughes & McLeod

Abstract

We selected 82 objects from the list of 2298 HII regions... to see if they contained radio sources. We selected half of them as objects with values of Y = log(S25/S12) >= 0.8, and half with values 0.3 >= log(S25/S12) <= 0.5. Of all the objects, 72% had at least one associated radio source, and total of 78 radio sources were detected.
... 

This catalog of 2293 probable HII region from IRAS PSC (old).
selection programs was wrote by S. Trushkin (SAO)

Criteria are from Hughes & McLeod (1989).
/*------------------------------------------------------*/
/*  criteria of HII regions in IRAS catalog:            */
/*  flux-quality numbers >= 1,2,2,1 at 12,25,60,100 mum */
/*  S(100mum) >=  50 Jy for FQ=2 or 3                   */
/*  S(100mum) >= 150 Jy for FQ=1                        */
/*  Y = log(S25/S12)  >= 0.0                            */
/*  X = log(S60/S25)  >= 0.0                            */
/*  Z = log(S100/S60) >= 0.2                            */
/*  -10 <= b <= +10                                     */
/*  confusion flags (hex) <=1 ( flag_c = 0, 1, 2, 4, 8 )*/
/*------------------------------------------------------*/
ex:
00494+5617 0049278+561728 15  9 45 31.807E+001.340E+013.296E+021.166E+031333 0
    0  5 12 11  268 19112251310640HAAA-1122365450000C93 47 43  123.065-6.309
22S184                266 552400 -29  14 Blitz CO HII f1=Diam'',f2=Vr,f3=Ta K
23MRSL 123-06/1       266 55 999 9992400 OhioStUn non-stellar objs f3=diam ''
23OCL 0313            303 46 999 999 960 OhioStUn non-stellar objs f3=diam ''
23CED 003             435 78 999 9991620 OhioStUn non-stellar objs f3=diam ''
  10  X=1.39 Y=0.87 Z=0.55

This is propable 949 PNs from IRAS PSC.
Hughes & McLeod (1989).

/*------------------------------------------------------*/
/*  criteria of PN  regions in IRAS catalog:            */
/*  flux-quality numbers >= 1,2,3   at 12,25,60,100 mum */
/*  Y = log(S25/S12)  >= 0.4                            */
/*  X = log(S60/S25)  <= 0.25                           */
/*  -10 <= b <= +10                                     */
/*------------------------------------------------------*/
ex:

00102+7214 0010168+721437 17  9 30 31.452E+017.190E+016.437E+012.686E+013332 3
81  4  4 11 12 173712242 5466  454BAAA 8080111200000873 33 34  120.016+9.868
 3RAFGL 5006           77293 999 999 -30 AFGL rev f1=4.2 ,f2=11,f3=17 mum mag
 7 NGC  40              4358 999 999   0 Stars with em.lines, f1=V mag,  f3=0
11PK 120+ 9.1          23 13 106 116  37 Strasbourg PN f1=V,f2=Bmag,f3=MinD''
   2  X=-0.05 Y=0.69