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The Astrophysical Journal, 225:40-55, 1978 October 1 .40B . .225. The Astrophysical Journal, 225:40-55, 1978 October 1 . © 1978. The American Astronomical Society. All rights reserved. Printed in U.S.A. 1978ApJ. H I, GALAXY COUNTS, AND REDDENING: VARIATION IN THE GAS-TO-DUST RATIO, THE EXTINCTION AT HIGH GALACTIC LATITUDES, AND A NEW METHOD FOR DETERMINING GALACTIC REDDENING* David Burstein Board of Studies, Astronomy and Astrophysics, University of California, Santa Cruz AND Carl Heiles Astronomy Department, University of California, Berkeley Received 1978 March 3; accepted 1978 April 5 ABSTRACT We reanalyze the interrelationships among Shane-Wirtanen galaxy counts, H i column densi- ties, and reddenings, and resolve many of the problems raised by Heiles. These problems were caused by two factors: subtle biases in the reddening data and a variable gas-to-dust ratio in the galaxy. We present a compilation of reddenings for RR Lyrae stars and globular clusters which are on the same system and which we believe to be relatively free of biases. The extinction at the galactic poles, as determined by galaxy counts, is reexamined by using a new method to analyze galaxy counts. This new method partially accounts for the nonrandom clustering of galaxies and permits a reasonable estimate of the error in log Vgal as a function of latitude. The analysis shows that galaxy counts (or galaxy cluster counts) are too noisy to allow direct determination of the extinction, or variation in extinction, near the galactic poles. From all available data, we conclude that the reddening at the poles is small [< 0.02 mag in E(R — V) over much of the north galactic pole] and irregularly distributed. We find that there are zero offsets in the relations between E{B — V) and H i, and between galaxy counts and H i, which are at least partly the result of an instrumental effect in the radio data. We also show that the gas- to-dust ratio can vary by a factor of 2 from the average, and we present two methods for correct- ing for this variability in predicting the reddening of objects which are located outside of the galactic absorbing layer. We present a prescription for predicting these reddenings; in the area of sky covered by the Shane-Wirtanen galaxy counts, the error in these predictions is, on average, less than 0.03 mag in E{B — F). Subject headings: galaxies: clusters of — interstellar: matter — radio sources: 21 cm radiation I. INTRODUCTION gas-to-dust ratio is variable, a phenomenon which has Despite many attempts to find a reliable method to previously been found by Seki (1973) in his study of measure the reddening of extragalactic objects, a the correlation between H i and galaxy counts and by UV observers in their studies of the interstellar generally accepted “best” method has not yet been medium (Jenkins and Savage 1974; Bohlin 1975; established. As shown in Paper I (Burstein and Heiles 1978), smooth esc \b\ models do not work well because Savage et al. 1977). Comparison of the galaxy counts of the patchiness of the interstellar dust. Ways to with H i column densities enables us to correct for the account for the irregularities in the reddening distribu- variable gas-to-dust ratio and to predict the value of E{B — V) with considerable accuracy. tion have centered on measuring either the variations in galaxy counts (e.g., Shane and Wirtanen 1967) or the H i column density (e.g., Knapp and Kerr 1974), II. THE DATA and then deriving a relationship between these extinc- Table 1 lists the galaxy counts (Agal) and the neutral tion indicators and the reddening. The previous large- hydrogen column densities (Ah) in the directions of scale investigation into the interdependence among H i, 49 globular clusters, 84 RR Lyrae stars, and two early- galaxy counts, and reddening (Heiles 1976) concluded type stars from Abt and Golson (1962). All of these that there were no simple relationships among these objects have \b\ > 10° and z distances larger than extinction indicators and produced some unresolved 300 pc. The galaxy counts are derived from the num- problems. bers given by Shane and Wirtanen (1967, hereafter In this paper we further investigate the relationship SW), corrected as in Heiles’s (1976) work. The units among these quantities and are able to resolve many are number per deg2, averaged over 13 deg2 centered of the problems. Most of them originated because the on each object; Agal is unavailable for objects with * Lick Observatory Bulletin, No. 807. 8 < —23° because of the southern limit of the SW 40 © American Astronomical Society • Provided by the NASA Astrophysics Data System .40B . .225. TABLE 1 . Reddening Data for Globular Clusters, RR Lyrae Stars, and Abt and Golson Stars: \b\ > 10° Object /II b11 E(B — V) Source Nu log JVsal R 1978ApJ. Globular Clusters—Southern NGC 104. 305.9 -44.9 + 0.04 1 246 NGC 362.. 301.6 -46.3 + 0.02 1,2 194 NGC 1261. 270.6 -52.1 0.00 1 114 NGC 2298. 245.6 -16.0 + 0.08 1 441 NGC 2808. 282.2 -11.3 + 0.25 2,3 502 NGC 5139. 309.1 + 15.1 + 0.11 1 425 NGC 5286. 311.6 + 10.6 + 0.28 4 680 NGC 5824. 332.6 + 22.1 + 0.14 5 432 NGC 5986. 337.0 + 13.3 + 0.17 4 638 NGC 6397. 338.2 -12.0 + 0.18 1 581 NGC 6541. 349.3 -11.2 + 0.18 1 461 NGC 6584. 342.1 -16.4 + 0.10 5 324 NGC 6637. 1.7 -10.3 + 0.20 1 499 NGC 6652. 1.5 -11.4 + 0.10 5 421 NGC 6715. 5.6 -14.1 + 0.17 3 434 NGC 6723. 0.0 -17.3 + 0.03 1,6 292 NGC 6752. 336.5 -25.6 + 0.04 1 226 NGC 6809. 8.8 -23.3 + 0.03 3 389 Globular Clusters—Northern NGC 288. 149.7 -89.4 + 0.03 7,8 123 NGC 1904. 227.2 -29.3 + 0.02 9 153 1.418 0.0 NGC 2419. 180.4 + 25.3 + 0.03 10 300 NGC 4147. , 252.8 + 77.2 + 0.02 1 140 1.757 + 0.5 NGC 4590. , 299.6 + 36.0 + 0.03 3 331 NGC 5024. , 333.0 + 79.8 0.00 1 148 1.663 ’ 0.0 NGC 5053. 335.6 + 78.9 + 0.03 11 117 1.664 0.0 NGC 5272. 42.2 + 78.7 + 0.01 1 46.2 1.878 + 1.0 NGC 5466. , 42.1 + 73.6 0.00 1 94 1.865 0.0 NGC 5634. , 342.2 + 49.3 + 0.03 5 188 1.447 -1.0 NGC 5694. 331.1 + 30.4 + 0.09 5 394 NGC 5897. 342.9 + 30.3 + 0.11 1 458 1.Ï79 ‘ 0.0 NGC 5904. 3.9 + 46.8 + 0.03 1 192 1.760 + 1.7 NGC 6093. 352.7 + 19.4 + 0.17 1,12 570 0.740 -2.0 NGC 6171. 3.4 + 23.0 + 0.30 1 745 0.700 -2.0 NGC 6205. 59.0 + 40.9 + 0.02 1 104 1.542 0.0 NGC 6218. 15.7 + 26.3 + 0.17 1 409 1.152 -1.0 NGC 6229. 73.6 + 40.3 + 0.02 5, 13 96 1.568 0.0 NGC 6254. 15.1 + 23.1 + 0.27 1.4 536 0.826 -3.0 NGC 6287. 0.1 + 11.0 + 0.40 5 798 0.342 0.0 NGC 6333. 5.5 + 10.7 + 0.37 5 849 0.204 0.0 NGC 6341. 68.4 + 34.9 + 0.02 1 144 1.657 + 1.0 NGC 6356. 6.7 + 10.2 + 0.40 1.5 904 0.114 0.0 NGC 6402. 21.3 + 14.8 + 0.37 14 747 0.114 -4.0 NGC 6864. 20.3 -25.8 + 0.17 5 468 NGC 6934. 52.1 -18.9 + 0.20 1 475 0Í9Í9 — 2.0 NGC 6981. 35.2 -32.7 + 0.07 1 251 1.294 -2.0 NGC 7006. 63.8 -19.4 + 0.10 1 391 1.187 + 0.5 NGC 7078. 65.0 -27.3 + 0.12 1 332 1.346 0.0 NGC 7089. 53.4 -35.8 + 0.06 1,3 220 1.387 -1.5 NGC 7099. 27.2 -46.8 + 0.06 1 214 1.767 + 2.0 RR Lyrae Stars + Abt and Golson Stars SW And. 115.7 -33.1 + 0.058 15, 16 327 1.656 + 1.5 XX And. 128.4 -23.6 + 0.035 15, 16 258 1.538 + 1.8 SX Aqr.. 57.9 -34.0 + 0.006 15 249 1.423 -1.0 TZ Agr. 53.2 -44.3 + 0.074 15 237 1.593 + 1.0 YZ Aqr.. 48.9 -49.8 + 0.064 15 230 1.800 + 1.5 BR Aqr.. 75.4 -55.2 + 0.024 15 202 1.501 -1.0 CP Aqr.. 48.7 -31.3 + 0.05 15 249 1.385 -0.2 DN Aqr. 35.7 -69.0 + 0.01 16 118 341 Aql.. 45.6 -22.0 + 0.034 15 401 1.ÓÍ7 -Ï.0 X Ari.... 169.1 -39.8 + 0.157 15, 16 684 1.356 + 2.5 TZ Aur.. 176.8 + 20.9 + 0.045 15, 16 331 1.493 + 3.5 ST Boo.. 57.4 + 55.2 -0.016 15 162 1.649 -0.5 SV Boo.. 68.8 + 65.5 + 0.024 15 99 1.555 -0.5 SW Boo. 62.5 + 67.8 + 0.007 15 24 1.693 -0.5 TW Boo.
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