The Number, Luminosity, and Mass Density of Spiral Galaxies As

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The Number, Luminosity, and Mass Density of Spiral Galaxies As The numb er luminosity and mass density of spiral galaxies as a function of surface brightness Stacy S McGaugh Institute of Astronomy University of Cambridge Madingley Road Cambridge CB HA ABSTRACT I give analytic expressions for the relative numb er luminosity and mass density of disc galaxies as a function of surface brightness These surface brightness distributions are asymmetric with long tails to lower surface brightnesses This asymmetry induces systematic errors in most determinations of the galaxy luminosity function Galaxies of low surface brightness exist in large numb ers but the additional contribution to the integrated luminosity density is mo dest probably Key words galaxies formation galaxies fundamental parameters galaxies general galaxies luminosity function mass function galaxies spiral galaxies structure Accepted for publication in the Monthly Notices of the Royal Astronomical Society Present address Department of Terrestrial Magnetism Carnegie Institution of Wash ington Broad Branch Road NW Washington DC USA INTRODUCTION The space density of Low Surface Brightness LSB galaxies has long b een a contro versial and confusing sub ject It is basic to our inventory of the contents of the universe and is crucial to many asp ects of extragalactic astronomy For example the density of LSB galaxies has an impact on the luminosity function faint galaxy numb er counts Ly absorption systems and theories of galaxy formation In this pap er I derive analytic expressions which quantify the density of discs of all surface brightnesses In order to clarify some of the p oints of confusion it is imp ortant to quantify what is meant by the term LSB Dierent p eople use it to mean dierent things leading to contradictory interpretations of otherwise consistent data One frequent but misleading use is treating LSB and dwarf as synonymous Dwarf galaxies may b e a subset of galaxies which are low in surface brightness but there exist many LSB galaxies which can not b e considered dwarfs either in terms of size or luminosity Romanishin Strom Strom Phillipps Disney Bothun et al Davies et al Imp ey Bothun Bothun et al Irwin et al Knezek Sprayb erry et al McGaugh Bothun de Blok van der Hulst Bothun a Some seem to refer to LSB galaxies as things which are totally invisible optically Others use the term to refer to any galaxy which is fainter than some canonical value like that of Freeman or the night sky In order to provide a consistent denition it is necessary to quantify the luminosity proles of galaxies Sersic found that the radial luminosity distribution could b e t by r h r e where is the central surface luminosity density in L p c h is a physical scale length in kp c and is an index which varies the shap e of the prole This is a generalization of the exp onential disc de Vaucoulers and r de Vaucoulers proles Since disc and bulge are b elieved to b e distinct physical comp onents and most debate concerns the numb ers of LSB disc galaxies I will limit the discussion to proles with ie spiral irregular and dE galaxies It is straightforward to generalise the results presented b elow for dierent prole shap es but in principle a multiparamter approach which adequately represents the full app earance of galaxies is required see McGaugh Bothun Schomb ert a In magnitude units the exp onential prole is r r where is the central surface brightness and is the angular scale length pro jected on the sky by a galaxy of physical scale length h at distance d The surface brightness and size of a disc galaxy are characterised by and h For pure disc systems is simply related to the eective surface brightness I will therefore use to characterise the global surface brightness of disc galaxies Using it is now p ossible to dene what is meant by low and high surface bright ness HSB Freeman asserted that all spiral discs had the same central surface brightness B mag arcsec This has b ecome widely known as Freemans law and is often used as a working denition of HSB To b e slightly more sp ecic I will dene as high surface brightness any disc with B mag arcsec which corresp onds to L p c Any disc which satises this criterion is likely also to fall within the narrow range sp ecied by Freemans law and the particular value is chosen to bracket it on the faint side On the bright side I will describ e as very high surface brightness VHSB anything which fails to ob ey Freemans law by b eing to o bright with mag arcsec or L p c The most obvious dividing line for dening LSB is the brightness of the night sky one magnitude fainter than the Freeman value in the b est of conditions To give a linear factor of two b etween this and HSB and to b e clearly fainter than the night sky let us describ e as LSB any disc galaxy with mag arcsec Fig shows examples of idealised high and low surface brightness galaxy proles Though I would prefer to avoid the p ollution of excessive nomenclature further quan titative distinctions are useful The transition region b etween HSB and LSB I will call intermediate surface brightness ISB since ob jects in this range do not ob ey Freemans law but are not particularly dim either It is also useful to denote the extremes of the LSB realm by very low surface brightness VLSB and extremely low surface brightness ELSB mag arcsec Most LSB galaxies which are known in the eld are to o bright for either of these categories though some examples do exist Nonetheless it is p ossible to see VLSB galaxies on survey plates if one lo oks hard enough It is not until the ELSB regime that galaxies b ecome eectively invisible to the deep est existing photographic surveys only one galaxy this faint has so far b een rep orted GP Davies Phillipps Disney The nomenclature utilised here is summarized in Table While such quantitative denitions are necessary to make sensible use of terms like LSB it should b e realised that there is some distribution of central surface brightnesses Obtaining this should b e our goal THE RELATIVE NUMBERS OF LSB GALAXIES To b egin in this direction it is p ossible to make a crude estimate of the relative numb er of galaxies in two widely separated surface brightness bins Recent surveys Schomb ert Bothun Schomb ert et al have identied large numb ers of LSB galaxies by visual examination of the plates of the new Palomar Sky Survey The selection criterion of the Schomb ert et al sample henceforth referred to as the LSB sample mimic that 0 of the diameter limited UGC Nilson The only dierence is the greater depth and lower grain noise of the new plates Ob jects are not included if already catalogued in the UGC Extending the UGC in this way will incorp orate galaxies which just missed the original diameter criterion This will include HSB galaxies which are on average slightly more distant as well as lower surface brightness galaxies In order to reject the former and isolate from the surface brightness distribution some p ortion which is truly LSB only galaxies were included which were essentially undetected on the POSSI This guarantees that only shallow prole LSB galaxies are selected Surface photometry of a subset of galaxies from the LSB sample shows that this pro cedure selects a p opulation which has a typical central surface brightness of B mag arcsec McGaugh Bothun de Blok et al a The distribution is very sharply p eaked around this value with a standard deviation of and a high kurtosis Note that is fainter than the Freeman value If Freemans law were correct and the surface brightness distribution really was a sharply p eaked function then these LSB galaxies should not exist Yet they represent an enhancement over the numb er of galaxies in the UGC Schomb ert Bothun and the UGC already contains a fair numb er of LSB galaxies Romanishin et al McGaugh Bothun de Blok et al a For a direct comparison to b onade HSB galaxies a sample is required which has surface photometry so that the adopted denition of HSB can b e quantitatively satised Such a sample exists in the data of van der Kruit who claimed to conrm Freemans law for large early typ e discs This HSB sample contains galaxies which have B mag arcsec the dierence b etween this and the Freeman value J b eing exactly comp ensated by the dierence b etween the B and B bands There are J 0 disc galaxies larger than over square degrees of sky of which were suciently face on to p erform surface photometry Of these qualify as Freeman discs the remainder b eing classied as LSB dwarfs Assuming that an equivalent fraction of the discs without surface photometry are HSB gives a surface density of Freeman discs of N p er HSB square degree 0 In comparison Schomb ert et al found LSB galaxies larger than over square degrees of sky Thirteen of these are classied as p eculiar ellipticals with shells or some other LSB extension leaving b ona de LSB galaxies Only seven of these are dEs the rest are spirals and irregulars Since dEs are low surface brightness and generally have exp onential proles I retain them but obviously this makes no dierence It is imp ortant that the sample consists mostly of spiral galaxies as it is often stated that Freemans law do es not apply to dwarfs This term is rarely quantied in this context and can follow from any of morphology size or luminosity The LSB sample do es not consist of dwarfs by any of these denitions The surface density of LSB spiral galaxies is N p er square degree LSB An
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