GENERATION OF COMPLETE SOURCE SAMPLES FROM

THE SLEW SURVEY

NASA Grant NAG5-1746

Semiannual Report No. 1

For the Period 15 August 1991 through 14 February 1992

Principal InvestigatorDr. Jonathan Schachter

February 1992

Prepared for:

National Aeronautics and Space AdministrationGoddard Space Flight CenterGreenbelt, Maryland 20771

Smithsonian InstitutionAstrophysical Observatory

Cambridge, Massachusetts 02138

The Smithsonian Astrophysical Observatoryis a member of the

Harvard-Smithsonian Center for Astrophysics*-•

The NASA Technical Officer for this grant is Dr. Donald K. West, NASA, Code 684.1,Laboratory for Astronomy and Solar Physics, Space Sciences Directorate, Goddard SpaceFlight Center, Greenbelt, Maryland 20771.

This report describes the status for the period 15 August 1991 to 14 Febru-ary 1992 of Astrophysics Data Program contract NAG5-1746 to the SmithsonianAstrophysical Observatory ("Generation of Complete Source Samples from theSlew Survey").

1 IdentificationsWe had proposed to establish well-defined samples of bright X-ray sources withthe Einstein Slew Survey, via identifications with optical counterparts. The SlewSurvey, which was 44% identified at the outset of the grant, is now 78% identified.These identifications have come from a thorough search of existing X-ray andoptical catalogs, SIMBAD, and the NASA Extragalactic Database. For sourcesnot previously known to be X-ray sources, nearly all (> 90%) of the proposedidentifications are consistent with X-ray to optical flux ratios from the EinsteinExtended Medium Sensitivity Survey. Only a small amount of optical observingis needed to confirm these identifications, since 80% of the unidentified sourcesare expected be brighter than V = 17.

We have searched radio catalogs (from the 6 cm 87GB and 90GB, theGreen Bank 20 cm, and the University of Texas 327 MHz surveys) to find possibleBL Lac candidates. These identifications will be confirmed by 22 hours of VLAsnapshot observations, which provide ~2 orders of magnitude improvement inradio flux sensitivity over radio catalogs, and few arcsecond positional accuracy.To help find optical counterparts, we have also searched digitized archives (theHubble Guide Star Catalog, the ROE/NRL UK Schmidt database, and theUniversity of Minnesota POSS plates).

We are developing statistical techniques to separate the correct counter-part from confusing foreground sources. Since X-ray sources are often muchbluer than field stars, we are using the MIT/SAO HEAO-Al U — B plates, andnew multiband UBV observations at Las Campanas (with M. Donahue). In aROSAT A02 collaboration with J. Truemper of MPE, we obtained positions,fluxes, and hardness ratios for all Slew Survey sources with ROSAT surveycounterparts. The factor of 3-10 improvement in positional accuracy over theSlew Survey will greatly aid our identification effort, while the PSPC to IPCflux ratios provide important variability and spectral information.

1

2 Data Products and Community InterestOver 100 members of the community have expressed interest in using the SlewSurvey data. We continue to receive requests monthly, and have made the SlewSurvey data products available in a variety of ways. A CD-ROM issued bySAO (Plummer et al. 1991) contains the full data on the individual photons inthe Slew Survey and the aspect solution file for each slew. (The CD-ROM wasfunded not by this contract, but by the Einstein data center grant.) This enablesa user to derive fluxes and upper limits for any position on the sky covered bythe Slew Survey. The CD-ROM also contains more information on the sourcedetections.

The CD-ROM has also been incorporated into the Einstein On-lineService, einline, which is accessible via modem or internet. In addition to theCD-ROM, users can search the Slew Survey source list at specified positionsdirectly in einline. The Slew Survey source list can also be accessed and searchedby the NASA High Energy Astrophysics Archive Research Center (HEASARC).Updated information on the Slew Survey is described in the semiannual HEAONewsletter, published by the SAO Einstein data center.

3 Scholarly Dissemination of ResultsThe basic techniques used to construct the Slew Survey are given in Elvis etal. 1992 (see attached preprint). This paper also contains a catalog of .positionsand optical and X-ray identifications. Our ongoing work is studying Slew Surveysource samples, and comparing to other existing complete samples. For example,the Slew Survey AGN are 3 magnitudes fainter in My than AGN in the PalomarGreen Survey (Schachter et al. 1992; see attached). Low-luminosity are thoughtto be the dominant contributor to the 2 keV X-ray background.

4 Slew Survey Bibliography and Discography

Elvis, M., Plummer, D., Schachter, J., & Fabbiano, G. 1992, ApJS, in press(May issue).

Plummer D., Schachter J., Garcia M., & Elvis M., 1991, CD-ROM issued bySmithsonian Astrophysical Observatory, Cambridge, MA.

Schachter, J. F., Elvis, M., Plummer, D., & Remillard, R. 1992, "ExtragalacticCounterparts to Einstein Slew Survey Sources," in Proc. X-ray Emissionfrom Active Galactic Nuclei and the Cosmic X-ray Background, in press.

EXTRAGALACTIC COUNTERPARTS TO

Einstein SLEW SURVEY SOURCES

JONATHAN F. SCHACHTER, MARTIN ELVIS, AND DAVID PLUMMERHarvard-Smithsonian Center for Astrophysics, MS 460 Garden St. Cambridge MA 02138, USA

RON REMILLARDMassachusetts Institute of TechnologyCenter for Space Research, Room 37-595Cambridge, MA 02139, USA

AbstractThe Einstein Slew Survey consists of 819 bright X-ray sources, of which 636 (or 78%)are identified with counterparts in standard catalogs. We argue for the importanceof bright X-ray surveys, and compare the Slew Survey to the ROSAT all-sky survey.Also, we discuss statistical techniques for minimizing confusion in arcminute errorcircles in digitized data. We describe the 238 Slew Survey AGN, clusters, and BL Lacobjects identified to date and their implications for logN-logS and source evolutionstudies.

1 Introduction1.1 Wanted: a Soft X—ray All—sky Survey

Before the ROSAT all-sky survey (RASS), no all-sky survey in soft X-rays was everperformed. For example, the well-known Einstein Extended Medium Survey (Stockeet al. 1992; see also Maccacaro in these proceedings) covers only ~2% of sky. All-skysurveys preferentially detect bright sources, owing to the large observed solid angleand the rarity of bright sources. The lack of survey information means that in the softX-ray band we paradoxically know more about faint sources than bright ones.

This has hampered our understanding of extragalactic X-ray sources. Atpresent it is necessary to compare Medium Survey results with those of the HEAO-A2 Piccinotti et al. (1982) sample in order to reach AGN with high fluxes and lowredshifts. Yet the normalizations of the soft X-ray and hard X-ray logN-logS areknown to be in disagreement from a Ginga fluctuations analysis (Warwick & Stewart1989).

1.2 Benefits of Soft X-ray Surveys

The steep luminosity function of AGN (meaning emission-line objects only) meansthat low luminosity AGN (e.g. Seyfert nuclei) are likely to provide a major part ofthe AGN contribution to the diffuse X-ray background (Schmidt & Green 1986). Yetoptical color-selected samples (e.g. the Palomar Bright Quasar Survey; Schmidt &Green 1983) are incomplete at low luminosities (My > —23) because of dilution byhost galaxy starlight. New X-ray-selected samples can be far more complete down tosignificantly lower luminosities (My ~ —18).

The second most important component in the 2 keV background is thoughtto be clusters of galaxies. Clusters have recently been observed in X-ray surveys toundergo negative luminosity evolution with redshift, i.e. there appear to be few high-redshift, high LX clusters in hard X-ray samples (Edge et al. 1990). and the MediumSurvey (Henry et al. 1991, preprint). The uniformly selected, unbiased cluster samplesof a soft X-ray all-sky survey can be used to compute a luminosity function to comparewith existing data.

1.3 IPC Surveys vs. the ROSAT Survey (RASS)

For a decade now X-ray logN-logS studies have been dominated by results from theEinstein IPC, a well understood instrument studied at the Deep (Primini et al. 1991)and Medium Survey flux limits. The energy range of the ROSAT PSPC is significantlylower than that of Einstein so that obscuration, both Galactic and intrinsic, is evenmore significant; thus, the population of sources ROSAT will detect will be biasedtoward softer spectra. These difficulties will enlarge the ambiguities in explaining thediffuse x-ray background since its spectrum is only well determined at energies wellabove the ROSAT energy range.

A tremendous effort is going on to identify ROSAT survey sources with opticalcounterparts. A master list of ~50,000 X-ray sources and positions has been prepared,but identification of all Medium Survey flux limit sources will require, plausibly,several years of optical observing and data analysis (see, for example, Bade in theseproceedings). In the interim before the ROSAT survey becomes available, we need asurvey to answer the important questions outlined above. For these reasons, we usedIPC data to construct an all-sky survey: The Einstein Slew Survey (see below). Ofcourse, when the ROSAT all-sky survey is fully identified, it will become a treasurefor X-ray astronomy into the 21st century.

lU |uVl . imi i - tptrlur. 1 bUll.UU.'.Jil

Figure 1: Spectrum of the serendipitous

V = 16 Slew Survey CV 1ES1113+432,obtained at MDM 1.3 m. Shows strongHa and weaker H/?.

{ (.DDE-It

6.00E-16

4.00E-16

2.00E-I6

4500 5000 5500 6500 7000

2 The Slew Survey2.1 Overview and Source List Revisions

The Einstein Slew Survey is an all-sky survey constructed from 2799 individual slewsof the IPC, and covering 50% of sky at an exposure of 6 s (Elvis et al. 1992). J Itcontains 819 bright soft X-ray sources ( £ 3 x 10~12 erg cm~2 s"1, 0.2 - 4.0 keV)with a positional accuracy of 1.2' (90% confidence radius), of which 317 were notpreviously known to emit X-rays. The flux limit is ~10-20 times higher than theMedium Survey. All the Slew Survey photon data, useful lists, and software tools areavailable either on CD-ROM (from the Einstein Data Products Office at CfA; email:edpo@cfa.harvard.edu) or via einline (telnet zahpod.harvard.edu, or 128.103.40.204;login as "einline").

Sources were detected by a percolation algorithm, which is more efficient thantraditional methods (e.g., sliding box) for a spatially sparse data set. For eachdetection, we calculated a Poisson probability that the distribution of photons isproduced randomly (PTand)- Initially we adopted logPran(/ = —3.95 as a threshold,which gave the list of 1067 sources on the CD-ROM. A much lower than expectedpercentage (60%; expected 80%-90%) of Slew Survey sources with RASS counterparts(with J. Truemper, T. Fleming, and W. Voges) led to a careful Slew Survey data re-analysis. The Slew/RASS comparison also provides important variability and spectralinformation, as will be detailed in a future paper. We subsequently have rejected asunreliable ~25% of sources, mainly with high Prand and low numbers of counts (3-5;details in Elvis et al. 1992).

2.2 New X-ray Identifications of Catalogued AGN and Clusters

Almost 80% (636) of the Slew Survey sources now have counterparts in standardcatalogs, from positional coincidences only. There are 136 new identified X-raysources (catalog counterparts with new Slew X-ray detections), which we have begunconfirming via optical observations. We have independently checked the assignedoptical counterpart type (e.g. AGN, BL Lac) of the new identified sources by comparingtheir X-ray to optical flux ratios with those expected from the Medium Survey (Stockeet al 1992). Most (84%) of the proposed counterparts have acceptable values of

'Due to the imminent publication of the Slew Survey Ap.J. Supplement paper, we will focus hereon results not discussed there.

ORIGINAL PAGE ISOF POOR QUALITY

H.SI8li»53? - Ap.rlur. I «0.00«~.pil

Figure 2: Redshifted MDM 1.3 m spec-

trum of the serendipitous Slew Survey

AGN 1ES1817+537 (z = 0.08). Ex-

hibits Balmer emission (Ho, H/?, H7) and

weaker O III AA4959, 5007. 4500 "5000 5500 6000 6500 7000

fx/fopt', the apparent disagreement for the remainder is may be caused by stars flaringin the Slew Survey, and AGN previously catalogued as normal galaxies.

Spectroscopy at the MDM 1.3 m has confirmed 17 counterparts and ruledout 8 others. The brightest Slew Survey source, at 10 IPC cts s"1 (or ~ 3.26 x10~10 ergs cm~2 s"1, 0.2-4.0 keV), is a serendipitous V = 16 CV (Figure 1). Wealso find 2 serendipitous AGN (1ES2137+241 at 2 = 0.05, and 1ES1817+537 atz = 0.08; Figure 2), and reclassify the catalogued normal galaxy ESO 509-14 asan AGN (z = 0.05). Echelle work by S. Saar at the McMath 2.5 m has discoveredstellar activity in bright, previously catalogued normal stars.

There are 124 Slew Survey sources with counterparts in catalogs of AGN, ofwhich 9 are new X-ray sources. We expect to get a total sample of 240-250 AGNwhen the Slew Survey is fully identified. To date, the highest redshift AGN in theSlew Survey is 4C 71.07 (= S5 0836+710; z = 2.2), a ROSAT AO2 PSPC target.The identified Slew Survey AGN to date are compared with the Palomar BrightQuasar Survey sample in Figure 3. Clearly, the Slew Survey can detect sources atleast 3 magnitudes fainter in Mv, showing the efficiency of detecting low-luminosityAGN. Plotting the Slew Survey and the Medium Survey AGN on a similar graph (notshown) shows that the two samples can be readily combined to sample a large rangeof luminosity-redshift space.

Figure 3: Redshift-V magnitude dis-

tribution for the Palomar Bright QuasarSurvey (O's), and for identified Slew Sur-

vey AGN to date (X's). The broaderdistribution in V magnitude for the SlewSurvey AGN is a consequence of the X-ray

selection. The Slew Survey AGN are seento be intrinsically 3 magnitudes fainter in

Mv.

1-1•8

-2

-3

Palomu- BQS (O's)va. Slew ACN (JTi)

12 u 16 isV Magnitude

20 22

We find 11 new X-ray clusters, of a total of 79 identified dusters; we expect160-170 clusters in the completely identified Slew Survey. The new X-ray clusters areall high z (or large £>), i.e. z >, 0.1, and also high LX, £ 1045 ergs s"1. If this trend

continues for the entire new X-ray cluster sample, it would contradict the negativeevolution found in other surveys, suggesting that the apparent evolution is due insteadto selection effects.

3 AGN Identifications from Digitized Plate Data3.1 Expected Optical Magnitudes

Most of the 183 sources with no counterparts in standard optical catalogs areexpected to be relatively bright. Using the known fx/fopt values and expected sourcedistribution (Stocke et al. 1992), we can divide the sources into 3 groups by expectedV-magnitude range: (i) V < 15. This group, containing 37% of the unidentifiedsources, is dominated by KM stars, (ii) 15 < V < 17. This group is dominated byAGN with some clusters as well. It accounts for 43% of the unidentified subset, (iii)17 < V < 19. The smallest of the three groups (20%), this has arguably the mostinteresting objects—BL Lacs and faint clusters. It is necessary to search digitized .plate data to find possible counterparts of these sources.

The digitized plate data we considered are the Hubble Guide Star Catalog(GSC; mv < 15), the POSS plates (mE < 22, mo < 21), and the southern UKSchmidt plates (mB(j) < 22). We concentrated on the GSC, since 90% of thesources with no counterparts in standard optical catalogs have GSC counterparts.This concentration also reflects issues of timing. As of 1991 October, the POSS platesare in the process of being scanned at the University of Minnesota, while querying theUK Schmidt database is an ongoing project at NRL.

3.2 Likelihood Techniques

To compensate for confusion (~ 7 x 102/sq. deg. at the GSC limit), we calculate thelikelihood of a positional coincidence relative to background—the likelihood ratio (e.g.,de Ruiter, Willis, & Arp 1977)—using source count estimates (Bahcall & Soneira 1980and Tyson & Jarvis 1979). We are testing likelihood techniques to identify sourcesin the Hubble Guide Star Catalog (GSC), using a subset of known identified X-raysources in the Slew Survey (mainly AGN and stars). Only 50%-60% of the knownsources match the GSC (i.e. within 1 mag). Intrinsic source variability, and poorhandling in the GSC of extended objects is probably to blame (e.g., Garnavitch 1991).However, we can study the number of known sources which do not match at all as afunction of likelihood. From these, a threshold likelihood of 3 was adopted.

Applying the likelihood technique to the GSC, we find 57 new optical identifi-cations of Slew Survey sources The dominant counterpart types are M stars (20, or ~35%) and AGN (16), which if confirmed spectroscopically bring the total AGN countto 140. We have begun to apply similar likelihood techniques to 103 digitized UKSchmidt (ROE/NRL) and 20 digitized POSS (U. Minn.) fields.

4 BL Lacs and Future WorkWe have identified 32 BL Lacertae objects to date, with 82 expected in the surveywhen fully identified. In addition, we have isolated 62 possible BL Lacs, from X-rayto optical and optical to radio flux ratios (Stocke et al. 1992). These will be observedin short 3.5 min exposures (to ~0.2 mJy) during a January, 1992 VLA run, where thegreatly improved positions will confirm or deny the proposed optical counterparts. Wewill also search the new southern 6 cm, 25 mJy survey (the PMN survey, currentlybeing reduced; A. Wright, priv. commun.), for BL Lac candidates. Currently, we arestudying IRAS to X-ray flux ratios as a way of separating different types of sources(Green, Anderson, & Ward 1992).

To further combat confusion, we have obtained BVR photometry of 17 uniden-tified Slew Survey fields at the Las Campanas 40" (with M. Donahue of MWLCO).Optical counterparts of X-ray sources are often significantly bluer than field stars andgalaxies (e.g., Remillard et al. 1992). We will continue this work in Spring 1992 at theCTIO Curtis-Schmidt.

This work was supported by NASA grant NAG5-1746 (ADP).

5 ReferencesBahcall, J. N., & Soneira, R. M. 1980, ApJS, 44, 73.de Ruiter, H. R., Willis, A. G., & Arp, H. C. 1977, AJ, 28, 211.Edge, A. C., Stewart, G. C., Fabian, A. C., & Arnaud, K. A., 1990, MNRAS, 245,

559.Elvis, M., Plummer, D., Schachter, J., & Fabbiano, G. 1992, ApJS, in press (April

issue).Green, P.J., Anderson, S.F., & Ward, M.J. 1992, MNRAS, in press.Garnavitch, P. 1991, Ph.D. Thesis, Univ. of Washington.Piccinoti et al. 1982, ApJ, 253, 485.Primini F.A., Murray S.S., Huchra J., Schild R., Burg R., & Giacconi R., 1991, ApJ,

374, 440.Remillard R., et al. 1992, in preparation.Schmidt M., & Green R.F., 1983, ApJ, 269, 352.Schmidt M., & Green R.F., 1986, ApJ, 305, 68.Stocke, J. T., Morris, S. L., Fleming, T. A., & Henry, J. P. 1992, ApJS, in press.Tyson, J. A. & Jarvis, J. F. 1979, ApJ, 230, L153.Warwick, R.S., & Stewart, G.C. 1989, in X-ray Astronomy, Proc. 23rd ESLAB

Symposium, ed. N.E. White (Noordwijk: ESA).

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Harvard-Smith son! aniaCenter for Ast rophys ics

Preprint Series

No. 3297(Received September 3, 1991)

THE EINSTEIN SLEW SURVEY

Martin Eivis, David Plummer, Jonathan Schachter, and G. FabbianoHarvard-Smithsonian Center for Astrophysics

To appear inThe Astrophysical Journal, Supplement Series

1992

HARVARD COLLEGE OBSERVATORYSesqulcentennial Year 1989

SMITHSONIAN ASTROPHYSICAL OBSERVATORYCentennial Year 1990

Center for AstrophysicsPreprint Series No. 3297

The Einstein Slew Survey

Martin Elvis, David Plummer, Jonathan Schachter, G. FabbianoHarvard-Smithsonian Center for Astrophysics

To appear in The Astrophysical Journal, Supplement Series, 1992.

Received: 31 May 1991; Accepted: 15 August 1991.

Running Title: The Einstein Slew Survey

ABSTRACT

A catalog of 1075 sources detected in the Einstein IPC Slew Survey of theX-ray sky is presented; 554 of the sources were not previously known as X-raysources. Typical count rates are 0.1 IPC count/s, roughly equivalent to a flux of3 x 10~12 erg cm~2 s~l. The sources have positional uncertainties of 1.2 arcmin(90% confidence) radius, based on a subset of 452 sources identified with previouslyknown point-like X-ray sources (i.e. extent less than 3').

Identifications based on a number of existing catalogs of X-ray and opticalobjects are proposed for 689 of the sources, | of the survey, (within a 3' error radius)including 170 identifications of new X-ray sources. A public identification data basefor the Slew Survey sources will be maintained at CfA, and contributions to thisdata base are invited.

Subject headings: surveys - catalogs - X-rays:general - X-ra.ys:stars -quasars:general - BL Lacertae objects:general

1. INTRODUCTION

Sky surveys have always played a major role in astronomy. In the presentera in astronomy we are rapidly accumulating new sky surveys across the wholespectrum. The advent of imaging telescopes has made X-ray surveys possiblethat are comparable in sensitivity to those at other wavelengths. The EinsteinObservatory (Giacconi et al. 1979a) was the first imaging X-ray astronomy satelliteand many papers have reported on surveys of restricted regions of the sky madeusing pointed observations taken with the Imaging Proportional Counter (IPC,Gorenstein et al. 1981) on-board Einstein. (The 'Medium Survey' e.g. Gioia et al.1990; the 'Deep Survey' e.g. Primini et al. 1991; Table 1). As a result we are inthe peculiar position in the soft X-ray band covered by Einstein (~0.2-3.5 keV), ofknowing more about the faint sources than about the bright sources. The limitedsky coverage of the Medium and Deep Surveys results in their having effectiveupper limits to their sensitivity as well as lower limits since bright sources are rareon the sky (figure 1; table 1). This limitation complicates logN-logS and sourceevolution studies (Figure 1) since for bright source counts we have to refer to thehard x-ray surveys, usually to the Piccinotti et al. (1982) HEAO-A2 survey whichcovered the 2-10 keV energy band. For example, Schmidt (1990) has emphasizedhow the Piccinotti et al. and the Medium Survey source counts are in contradictionfor AGN and clusters of galaxies (although evolution may explain these problems,Gioia et al. 1990). What is needed is a logN-logS with the same instrument overthe whole x-ray flux range. A survey of the bright sources in the soft x-raj- range isthus important and only a survey covering most of the sky can find the relativelyrare bright sources. A survey using the same instrument as used for the EinsteinMedium and Deep Surveys would greatly simplify interpretation. Samples of brightsources selected uniformly by their X-ray properties are also valuable for follow-updetailed work with other instruments, e.g. ROSAT, ASTRO-D.

We have constructed a survey of the sky with the Einstein IPC using the'Slew' data taken when the satellite was moving ('slewing') from one target to thenext. By co-adding all these slews we have achieved a useful sensitivity over alarge solid angle, some 50% of the sky. The main properties of the Einstein IPCSlew Survey are given in table 2. Because it was not clear that this survey couldbe constructed successfully it was not attempted earlier. The resources needed toprocess the data were large, making the effort too large for the uncertain payoff.Computer processing power and on-line storage capacity have grown by orders ofmagnitude in the last few years so that it is now possible for projects of this sizeto be carried out experimentally by a small team relatively quickly, and thus atlow risk. This paper describes the Einstein Slew Survey and presents the resultingcatalog of X-ray sources.

The complete information content of the Slew Survey is more than the sourcecatalog. A CD-ROM issued by SAO (Plummer et al. 1991) contains the full dataon the individual photons in the Slew Survey and the aspect solution file for eachslew. This enables a user to derive fluxes and upper limits for any position on thesky covered by the Slew Survey. The CD-ROM also contains more informationon the source detections, (see 'lists/unix/srcs.lis', 'lists/vms/srcs.lis' etc.). TheCD-ROM is available from SAO (send requests by e-mail to the Einstein DataProducts Office, edpo@cfa.harvard.edu), or via the Einstein On-Line InformationSystem, em/me (Harris et al. 1991).

2. DATA SELECTION

For the survey we selected all the data taken while the Einstein satellite wasslewing with the IPC at the focus ('SLEW mode data- hence the survey name).Only the IPC data is valuable for this survey. Table 3 compares a 'figure of merit' forthis type of work for the four focal plane instruments on Einstein. The combinationof wide field of view, high quantum efficiency, and large fraction of time in the focalplane combine to make the IPC over 100 times more valuable than the next mostuseful instrument, the HRI. Only slews for which IPC targets lay at each end wereused (i.e. no instrument changes during the slew). Also only slews in which whichdata dropouts were small (< 1 major frame, 40.96 s) were included. This gave 2799useful slews with a total instrument on-time of 1.0 million seconds of data, and 2.6million photons.

All photon events were accepted: unlike the processing of the pointed data noSun/Earth angle or pulse height event (PHA) screening was made. Screening provedunnecessary for most of the survey since its purpose is to reduce the background,which is negligible for the short exposures in the Slew Survey. In processing weomitted photons from regions near the IPC 'ribs' (features produced by the windowsupport structure of the IPC, Harnden et al. 1984), and near to the edges of thedetector. Edge photons are not processed in the standard, pointed, data either.

Figure 2 shows the exposure map for the Slew Survey. The concentration ofexposure near the ecliptic poles is clear. This concentration occurs for all Earth-orbiting satellites with fixed solar panels since one axis must point toward the Sunand the satellite lies in the ecliptic plane. The spacecraft is then only free to rotatealong arcs of ecliptic longitude. There is lower than average exposure in parts of theGalactic plane, because the IPC was turned off if it was expected to slew across thebrightest few sources, and these are concentrated in the Galactic plane. This wasa protection against detector gas breakdown that could be induced by too manycounts being detected in a small region. The Slew Survey thus has zero exposureon the Crab Nebula. This policy was not always successfully followed and we do

have exposure on GX5-1, which was fortunate for our purposes since it allowed a'proof-of-concept' at an early stage (figure 3).

Figure 4 is an exposure histogram showing the fraction of the sky covered toa given exposure depth. From this, and the logN-logS of the Medium Survey (Gioiaet al. 1990) one can predict that the Slew Survey will contain of order 1000 sources,which in fact is a quite accurate prediction.

3. ASPECT SOLUTION

The key to producing a Slew Survey is to solve for the pointing position ofthe satellite with time as it slews across the sky (the 'aspect' or 'aspect solution').To determine the Einstein aspect during slews it was necessary to use the on-boardgyroscope rate data ('gyro data'). The on-board star trackers, which are the primarymeans of providing the aspect solution for the pointed observations, could not beused since the satellite moved some 5-6 ' during a single readout interval (1 minorframe = 0.32 s, the standard minimum read-out interval for a NASA mission), whilethe star trackers could only follow stars at rates of <2 arcminutes s"1 (Koch et al.1978).

At any time during the mission three of the six gyros in the gyro assemblywere operating. Each gyro yields a spin rate every minor frame, and the gyrosare oriented so that any set of three will give sufficient information to determinerotations about the three spacecraft axes. The existing calibration of the gyro ratesto rotation rates was designed only to be accurate enough to bring the spacecraftto a direction where the star trackers, with their ~ 2° field of view, could acquire afield. Accurate pointing depended on the star trackers.

To use the gyros alone for deriving a Slew aspect required that the existingcalibration be checked, and modified to give solutions accurate at the arcminutelevel anywhere during a slew. Two things made this possible: (1) the level ofaccuracy required is of order 1'—similar to the IPC point spread function—whichis some 30 times less demanding than for pointed observations; and (2) enoughwell-positioned X-ray sources are known which are bright enough to be detected ina single slew. These sources give us an internal check on the quality of our aspectsolution on several hundred individual slews, thus allowing a reliable Slew aspectsolution to be developed.

Figure 5 shows the initial offsets between the slew derived position and theaccurate positions for known X-ray sources in the HEAO-1 A3 (Remillard et al.1991) and pointed IPC catalogs (2E; Harris et al. 1991) detected in individualslews. The coordinates are oriented along and perpendicular to the slew direction.Several features can be seen: There is a concentration of points near the origin,

implying that a good fraction of the time the gyro system does give good aspectduring slews; this concentration is however offset along the slew direction by ~3-5' ; there is a 'tail' of poorly positioned sources along the slew direction; and there isa 'halo' of poorly positioned sources extending to large distances from the centralcluster near the origin.

The offset of the central cluster is due to an ambiguity in the documentationof the timing information. We determined empirically that the aspect data andphoton data sent in a single data packet (minor frame) refer to different times: thephoton data to the current minor frame and the aspect data to the preceding minorframe. This is negligible in pointed mode but in Slew mode leads to the observedoffset.

The 'tail' of poor aspect slews we found to be due to the quality of the pointedaspect at the start of the slew. The 'MAPMODE' star tracker aspect (where thetrackers send back the positions of all stars in the field) is not sufficiently reliable(e.g. Harris, Stern and Biretta 1990a) and it is essential to go back into the pointedobservation until 'LOCKED' star tracker aspect is found. (In LOCKED aspectthe tracker records only the position of the chosen guide star.) Errors of a fewarcseconds in the starting position extrapolate to large errors when the spacecraftslews through tens of degrees.

The cause of much of the spread seen in figure 5 is seen in figure 6a. Thisshows the offset perpendicular to the slew direction as a function of position alongthe slew path. The clear 'bow' shape arises naturally from a displacement of thegyro assembly from its assumed orientation with respect to the spacecraft axes.This offset can be illustrated by imagining a vector rotating 180° within a givenplane. This represents the actual rotation of the satellite. Now consider a secondvector parallel to the first vector at its original position. Rotate the second vectorwithin a second plane tilted slightly from the first plane such that they intersectalong the line of the vectors' original direction. The second vector represents therotation of the satellite as reported by the displaced gyros. The two vectors will becoincident at the start and end of the 180° rotation, but will be offset in between,reaching a maximum at 90°. The offset at 90° exactly equals the relative offsetof the two planes, and therefore the offset of the gyro assembly. By rotating thegyro assembly axes according to the maximum observed offset the 'bow' distortionsin the derived positions can be virtually eliminated (figure 6b). A separate set ofcorrections is needed for each set of gyros which indicates that the rotations arenot of the gyro assembly as a whole but of the individual gyros mounted in theassembly. Errors in the assumed gyro orientations of a few arcminutes are entirelynegligible for pointed observations. The rotations for each set of gyros were fixedand are given in table 4.

In addition the conversion from gyro spin rate to angular rotation is onlycalibrated to a level sufficient for pointed operation. In the Slew Survey thisconversion is critical, and leads to errors when extrapolating the gyro solution overlarge slew angles. We calculate the initial offset between the known, star-tracker-derived, pointing position and the gyro-extrapolated position at the end of the eachslew. Each offset is measured as a small difference, 6, in R.A., Dec. and Roll angle.Since we measure three £'s and can adjust the scale factors for three gyros there issufficient information to force this offset to be zero for each slew. The correctionsneeded are of order 3'. We used the following procedure: using the initial offsetswe guess an appropriate trial scale factor for each gyro in turn. This leads to achange in the three £'s for each of the three gyros. The resulting 3x3 matrix formsa set of simultaneous equations which can be solved to give scale factors for eachgyro that will exactly set the £'s to zero. This procedure produces a sufficientlyaccurate aspect solution, as determined, post facto by the identification process (see§6). The scale factors, however, are mostly not systematic. This suggests that thereis a residual aspect error that could, if corrected, improve the Slew Survey aspect.The solution may lie in treating the orientation of each gyro separately instead of'rotating' the whole gyro assembly.

Finally slews having scale factor corrections larger than 2% were found tointroduce greater errors in position. In very short slews, for example, the aspectbecame so bad that sources were distorted into smears that were not detected at all.We simply excluded any slews for which we derived scale factor corrections largerthan 2% (8.6% of the total), leaving the total of 2799 useful slews.

The offsets of the Slew positions from the accurate positions of known X-ray sources in the HEAO-1 A3 catalog (Remillard et al. 1991) and the BrightStar Catalog (Hoffleit and Jaschek 1982) for the final set of corrected aspect slewsgave the offset diagram seen in figure 7a. The true reliability of the Slew Surveyaspect solution is better than is immediately apparent from figure 7a since falseidentifications produce a significant 'background' at radii >3'. Figure 7b shows thedistribution of offsets from a false set of Slew Survey sources obtained by shiftingall the Slew Survey sources by 1° in R.A. Figure 7c shows a plot of the averagebackground due to false identifications plotted against the radial histogram of figure7a. Subtracting this background rate implies a 90% confidence radius of order anarcminute for the Slew Survey aspect. Figure 7d shows an integrated histogramwith the background subtracted which allows the derivation of confidence radii ofthe reader's choice. We derive a 90% confidence radius of 1.2' and a 95% radius of3'from figure 7d.

4. SOURCE DETECTION

The short exposures of the Slew Survey over most of the sky lead to anexpectation value of 0.1 photons in a standard 2.4' square IPC detection cell. Sincewe expect ~1000 sources over the sky, approximately 99.996% of the 2.58 x 107

detection cells would be empty of sources. The 'sliding box' detection algorithmused for the pointed data (Harnden et al. 1984) is thus highly inefficient for the slewsurvey.

4.1 Percolation Algorithm

Instead we have developed a 'percolation' algorithm that tests each photonfor the presence of unusual numbers of near neighbors. Since there are only ~ 3 x 106

photons in the survey this takes a factor of ~ 50 fewer operations than the sliding boxmethod. The percolation algorithm is exactly analogous to the method describedby Huchra and Geller (1984) for the selection of groups of galaxies from the CfARedshift Survey (Bright galaxies, like Slew Survey photons, are sparsely distributedon the sky) except that the Slew Survey contains only the two dimensions ofR.A. and Dec., and has no equivalent of the redshift dimension. The Slew Surveypercolation algorithm loops through every photon in the field and searches for otherphotons within the percolation length. If another photon is found it is added tothe group and subsequently searched for neighbors. The process continues until nomore photons lie within a percolation length. Figure 8 describes the process in aflowchart. These groups constitute our candidate sources for the Slew Survey. Thisalgorithm has the advantage of not being biased against extended sources as is asliding box (by subtracting a source-enhanced background). It does, of course, havea surface brightness limit when the mean distance between source photons exceedsthe percolation length. A percolation length of 2' (~ double the FWHM of the IPCpoint spread function) produced good results except in regions of high exposurewhere the background began to become important (see below). All groups detectedby the percolation algorithm with fewer than three photons were automaticallyrejected.

4.2 Exposure Map

It was then necessary to determine which photon groupings constitutedsignificant sources. This significance is highly dependent on the local backgroundand the distribution of exposure time around a source. Figure 9 illustrates some ofthe difficulties. The contours are iso-exposure levels. Each field covers 30x30' andthe exposure map has a resolution of 1'. Detailed structure on the few arcminutescale is evident. Because of the random nature of the slew paths there is no

8

predictable structure to the exposure maps. Figure 9 also shows the individualphotons in the regions. Each frame is centered on a Slew Survey source whichillustrates that the size of the point spread function is comparable with the exposuremap structure. It is clear that the detailed exposure distribution in the surroundingregion must be calculated in order to compare the background from this region withthe number of counts detected in the 'source' region defined by the percolation detectalgorithm.

The exposure maps were generated from the aspect solution and the timinggap records ('.tgr' files) for each slew ('HUT'). A template of the relative exposurewithin the one degree IPC field of view was made including corrections for vignettingand window support features ('ribs', Harnden et al. 1984) at the full 8" resolution ofthe detector. The vignetting is a radial function which reaches 46% at the midpointof the side of the IPC; the regions affected by the ribs (which are 4' wide and roughly20' from the center, parallel to the sides, see Harnden et al. 1984 for details) are setto zero exposure. This map was then moved across the sky at the rate determinedby the aspect solution and effective exposure time assigned to one arcminute squarebins on the sky accordingly. For convenience the sky was divided into a set of 6.5°square bins on 6° centers. No exposure was accumulated during times when thedetector was off, or data was not received for other reasons (e.g. telemetry dropout).

4.3 Source Probabilities

The Poisson probability of a collection of 'source' photons arising by chanceinside a source region centered on the percolation centroid can be calculated givena local background. Source counts were derived by taking all counts within a 6' ona side box centered on the centroid given by the percolation algorithm. Backgroundwas estimated from two 'square annuli1 of inner side 6' outer side 12' and inner side12' outer side 30' (background regions 1 and 2). The mean exposure times in thesource and the background regions were derived by averaging the one arcminutebins of the exposure map. In the case where there were no background countswe calculated the probabilities by assuming one background count. Otherwise, weused background region 2 for background subtraction. The probability, PTand, wasdetermined for each candidate source. (On the CD-ROM Prand is called Prob2;Probl, the same probability using the background region 1, was also calculated andis listed on the CD-ROM.) The values of Prand order the candidate sources accordingto their likely reality (small probabilities being more likely real). Prand does not byitself tell us which sources to accept. For this we must define a threshold value of

4.4 Setting the Threshold Probability

Setting a threshold probability for source acceptance is a balance betweenexcluding too many real sources and including too many false sources. We adoptedtwo methods for determining an appropriate threshold. The first predicts theexpected number of sources based on Poisson statistics; the second checks thereliability of the sources by the distribution of positional offsets for identificationswith optical counterparts.

We can predict the expected number of false sources. We first used thedistribution of single photon 'source candidates' since these are the least likelyto be real sources. Figure 10 shows a histogram of the number of single photoncandidates as a function of PTand- The histogram peaks at a probability of 0.5 wherethe number of 'source' photons equals the number of background photons, which isthe most likely case. (Above a probability of 0.5 our sample will necessarily alwaysbe incomplete because the percolation algorithm cannot include candidates withzero counts in the source box.) If the probability calculation is appropriate to thedata then we should find that the number of candidate sources drops linearly withprobability. We show a straight line of slope 1 in figure 10 which was normalizedby setting the area under the line equal to the area under the histogram up to aprobability of 0.5. This normalization assures that the line intersects the histogramat Prand ~ 0-5. Since the line fits the data well for about four decades in probabilitywe conclude that the Poisson probability is a good description of the data. This is aconservative approach because we are assuming that the percentage of 'true' sourceswithin the total sample is essentially zero, whereas some single photon 'sources' willindeed come from real sources.

We can then use this predicted distribution of false sources with the list of'candidate sources' (those with three photons or more) to determine the number offalse sources as a function of PTand- The histogram of figure 11 shows the numberof sources detected as a function of PTand- The solid line was normalized as forthe single photon candidate sources to give the same area under the curve as thehistogram, up to Pr0n<f=0.5. The line then predicts the number of 'false' sourcesincluded as a function of Prand- A convenient representation is given in figure 12which shows the percentage of false sources as a function of the Prand threshold.

We selected a value of log(PTan<i} = 3.95 as our threshold. This criterionyields a list of 1085 prospective sources with 21 false sources expected to be included,~ 2% (see figure 12). If the statistics were Gaussian this would correspond to a3.3cr threshold; but the highly asymmetric nature of the Poisson distribution forsuch small numbers of counts makes the detections more significant that commonexperience with 3cr results would suggest.

Figure 11 shows an excess of candidate sources even above our thresholdprobability, implying the existence of many real sources up to quite high Prand,

10

as one would expect. Some of these sources may be extractable by searching theoriginal Slew Survey data at a predefined set of positions such as those of an opticalcatalog. This is possible given the software and data on the CD-ROM (Plummeret al 1991).

The source list (see §6) gives the values of Prand for each source so thatreaders may set more stringent thresholds if they wish. We believe that our visualcheck (below) has probably removed of order half of the false sources.

An independent check on the level of confidence we can place in the final listof sources is given by the following procedure. We have made identifications of all thecandidates against two catalogs of known X-ray sources that have positions knownto better than one arcminute- the Einstein IPC Catalog (2E, Harris et al. 1991)and the HEAO-A3 Catalog (Remillard et al. 1991). Figure 13 shows the offset ofthe Slew position from the known position in arcminutes for sources matched in thisway, against the probability of the source being a chance congregation of photons,PTand • Extended sources, (clusters of galaxies, supernova remnants and all otherIPC sources with 'extent parameter' > 3') were excluded from this comparison.

It is clear from figure 13 that for small probabilities (Pra.nd < 10~6) almostall the sources must be real since they are clustered at offsets of order theaspect accuracy derived from individual slews. Similarly at large probabilities(Prand > 10~3) there are a great number of false sources since they are distributednearly uniformly in offset. Our threshold Prand for accepting a candidate source asreal is clearly at a level where the fraction of identified sources lying within 2' ofthe optical position begins to decrease rapidly, as one would expect from figure 11where the fraction of false sources is low (>90%) until Prand ~ 10~4, and then risesrapidly.

As a final check, two of us (M. E. and J. S.) visually inspected each ofthe proposed sources for cases of dubious detections. A total of 10 sources wereeliminated in this manner. Of these 8 were rejected because photons from the outerfringes of a bright source caused a spurious second detection; 2 were rejected becausethe exposure gradients across the region were extreme and an isolated region of highexposure led to a 'source'. A reliability index (1, 2, 3; 3 best) was compiled basedon the visual inspection (see §6).

In Figure 14, the fraction of objects within 2' of the correct position is plottedagainst the probability of a source arising by chance. Note that the figure containsan excess of sources near to zero offset even at Prand > 10~3 which is consistent withfigure 12. This implies that other real sources exist in the data. Searches of theSlew Survey data base at given positions, defined a priori by e.g. a optical catalogmay give significant detections even if no source appears in this catalog. (Since the

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number of trials is small a lower significance threshold can be used.)

4.5 High Background and Extended Sources

As noted above in regions of high exposure the percolation algorithm did notproduce sensible results because the mean distance between background photonsbecame similar to the percolation length. Thus large areas of background wereincluded with sources, leading to large extended 'sources'. This tends to mergesources together and leads to their systematic undercounting in these regions. Wedealt with this problem by selecting all sources with a maximum photon distancefrom the percolation centroid of > 9'. We then reran the percolation algorithm witha smaller percolation length, which normally resolved the problem. Figure 15 showshow the galaxies M81 and M82 were initially included in a single source, but wereresolved by using a shorter percolation length.

We found that when Probl/Prob2 (defined in §4.3) is large ( > 103) thesource is extended, or that there are multiple sources within 15 arcmin. A visualinspection of all cases with Probl/Prob2 > 103 was made (M. E. and J. S.). Forall such sources an 'Image Code' was assigned which notes extended sources largerthan ~15' (E), regions with multiple sources within 15' (M), and sources which area part of a larger extended source (P). Sources with acceptable Probl/Prob2 areassigned the code 'A'.

Some sources are truly extended on this scale. Each extended sourcewas inspected visually, which we found to be an effective, but unfortunatelysubjective, means of discriminating real sources from confusion with background.This procedure added 33 sources and improved the positions of 78. A moreautomatic means of changing the percolation length with the exposure to matchthe mean free path between background photons needs to be developed. Some fewsources have extent of order degrees (e.g. the Cygnus Loop, Puppis A). Althoughthese are not included in our source catalog the data is on the CD-ROM. Thesesources will be treated fully in a later paper (Schachter et a/. 1991, see also §7).

5. SOURCE PROPERTIES

Having produced a list of reliable sources we need to determine theirproperties. The IPC gives information on positions, count rates, structure, andpulse height (energy).

The reliability of the positions was established using known X-ray sources,as described above (§3, figure 7c).

Count rates were derived from the 6' diameter box used for the probability

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calculation with background from background region 2 (see §4.3).

For extended sources (e.g. clusters of galaxies, supernova remnants, and thoselabled 'E' in the source table) the count rates will clearly not be accurate. For mostof these a better count rate can be derived using the counts and exposure in the6'-12' 'square annulus' surrounding the central detection cell (background region1). This information is available on the CD-ROM version of the Slew Survey (see'lists/unix/readme.txt', 'lists/vms/readme.txt.' etc.).

The count rates were checked for accuracy by comparing the Slew Surveyrates with those derived from the pointed IPC data for sources in common. Infigure 16a we plot the Slew Survey count rates as listed in this catalog versus thepointed IPC count rates from the 2E catalog (Harris et al. 1991). There is a strongcorrelation with a slight offset (a factor 1.19) toward higher count rates in the SlewSurvey. This is due primarily to our use of all 15 PI bins in the Slew Survey,compared with the standard 2-10 used in pointed data. (The restricted range forpointed data is used to minimize background, which is unnecessary in the SlewSurvey.) When we restrict the Slew Survey source count rates to the same PI binsthe offset is reduced to a factor 1.03, as shown in figure 16b. The source of thisresidual offset is still under investigation. The errors on these count rates are non-trivial to determine since both the background and the source counts are not inthe Gaussian limit and so do not add in quadrature. The problem of calculatingthese uncertainties in the Poisson case has recently been investigated by Kraft et al.(1991) and we have used their methods with software routines which they kindlysupplied to us. (Note that the uncertainties on the CD-ROM assumed Gaussianstatistics. Updated values can be obtained using em/ine, Harris et al. 1991)

Several measures of source extent were attempted. Large sources, >9'diameter, are readily selected using the maximum distance of a source photon fromthe percolation centroid. Smaller extended sources are clearly seen on the maps butare not so easily characterized. We are continuing a search for an objective meansof classifying the size of sources.

The mean pulse height bin for each source was calculated from the photonsin the 6' box. The 'pulse height invariant' (PI) bins were used since they have afirst order correction to remove the effects of the variable gain of the IPC (Harndenet al. 1984). (This variation changes the mapping of photon energy to pulse heightbin.) That an extreme ultraviolet source from the Wide Field Camera on ROSAT(1ES1631+781) has a mean PI bin of 2 (on a scale from 1, low energy, to 15, highenergy) shows that the PI data carries useful information.

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6. SOURCE LIST

The Slew Survey source catalog contains 1075 sources. l Table 5 gives asummary of the identifications made.

6.1 Table of Objects

Table 6 is the Slew Survey source catalog. The identifications suggested intable 6 are discussed in the next section (§7). Table 6 has the following entries:

Column 1: SOURCE NAME. '1ES' stands for first Einstein Slew Surveysource. Coordinate names are based on the B 1950.0 position constructed fromhours,minutes±degrees,tenths of degrees, truncated according to the IAU conven-tion.

Columns 2 and 3: POSITION. In B1950.0 coordinates, based on the percolationalgorithm centroid. Where noted positions have been refined by changing thepercolation length as discussed in §4.5. Errors on position are primarily systematic,arising from the aspect solution. A 90% error radius of 1.2' and a 95% radius of3.0' are estimated from figure 7d.

Column 4: COUNT RATE. Mean count rate in all PI bins (1—15). This is onaverage a factor 1.19 larger than the standard IPC 'broad band' count rate (basedon PI channels 2—10) used in the 2E catalog (see §5). Counts are taken from a 6'on a side box centered on the percolation algorithm centroid. Background countsscaled for exposure and area from a 30' on a side box (background region 2) havebeen subtracted. Errors represent a 1 a confidence interval. When total sourceplus background in the source box had <100 counts the error bars are based ona Poisson probability, distribution as computed in Kraft et al. (1991), which givesasymmetric error bars. For sources with a larger number of photons a Gaussianapproximation was used.

Column 5; NUMBER OF PHOTONS (NP) in the 6' on a side box and NUMBEROF SLEWS (NS) that contribute photons to the object. Other slews may havepassed over the source positions but yielded no photons.

Column 6: PROBABILITY, Pran<f. Probability of finding the number of photonslisted in column 5 relative to background region 2. Small numbers indicate a higherchance that the source is real. Values of PTand < 1 x 10~10 are listed as equalto 1 x 10~10. A threshold of log(Pranj) = —3.95 was used to generate the list ofaccepted sources.

JThe CD-ROM contains 8 fewer sources due to a software bug which omitted a thin slice of R.A.near 24h.

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Column 7: EXPOSURE. Total Slew Survey exposure time averaged over the 6' ona side box used in column 3.

Column 8: MEAN PULSE HEIGHT bin. The average of the 'pulse invariant'(PI, Harnden et al. 1984) channel numbers (1-15) for each photon, which coarselyindicates the source spectrum.

Column 9: QUALITY CONTROL INDEX (Q) and IMAGE CODE (I). The Q (1,2, or 3; 3 being highest quality) value is a visual estimate of the reliability of thesource. The IMAGE CODE highlights cases where Probl/Prob2 (defined in §4.3)is large ( > 103), and which a visual inspection shows to be extended, or to havemultiple sources within 15 arcmin (see §4.5). The IMAGE CODE has the followingvalues:A — Generally acceptable Probl/Prob2;E — Extended source (> 15 arcmin);M — Multiple sources within 15 arcmin;P — Part of source (extended source existing in more than one field).

Columns 10 and 11: EOSCAT NUMBER, Einstein MEDIUM SURVEY MEM-BERSHIP (noted by m), and OFFSET FROM EOSCAT POSITION (A2E). Forsources with counterparts in the 2E Catalog (Harris et al. 1991), we provide theEOSCAT number and the difference between the Slew Survey and catalog positions,in arc minutes. In addition, Medium Survey (Gioia et al. 1990, Stocke et al. 1991)sources are noted with a letter m preceding the EOSCAT number.

Columns 12. and IS: HEAO—1 A3 COUNTERPART, EXOSATDETECTIONS(noted by z), and OFFSET FROM HEAO—A3 POSITION (A1H). For sourceswith counterparts in the HEAO—1 A3 catalog (Remillard et af.1991), we providethe '1H' name and the difference between the Slew Survey and catalog positions, inarc minutes. In addition, EXOSAT sources are noted with a letter z preceding the1H name.

Columns 14—17: OPTICAL CATALOG (Cat.), OBJECT CLASSIFICATION(Class.), COUNTERPART NAME (Name), and OFFSET FROM CATALOGPOSITION (AC). For sources with counterparts in (mainly) optical catalogssearched to date (see below for catalog list and references), we provide the name ofthe catalog, the classification (e.g., AGN), the counterpart name, and the differencebetween the Slew Survey and catalog positions, in arc minutes. If the redshift orstellar spectral type is known, it is listed after the object classification in column15.

Composite spectral types in table 6 indicate a binary (or other multiple starsystem). In general, we have tried to use the most common names of objects.For cases in which two objects (most commonly an SAO star and an extragalactic

15

object) were found in the same error box we compared their fx/f0 ratios with thosefor the Medium Survey sources (Maccacaro et a/,1988). In most cases only oneof the objects was a plausible counterpart given these ratios. Cases in which morethan one object is a likely counterpart are indicated with asterisks, and noted below(§7-3).

If the counterpart name is the same as the Slew name in column 1, and thecatalog is well known, only the catalog designator is listed in column 16 (e.g., PG,EXO, 2E). Woolley names with letters A, B, ... indicate multi-star systems (e.g.,WLY 127AB). For each of the newly discovered X-ray sources, we list all the namesknown to us in Table 7.

Abbreviations for names of catalogs are:2E—Second Einstein IPC Catalog ('EC-SCAT, Harris et al. 1991);A3—HEAO—A3 Catalog (Remillard et al 1991);ABL—Abell Catalog Abell Catalog (1958, Struble and Rood 1987) and SouthernAbell Catalog (Abell, Corwin, and Olowin 1989);BMC—Bradt and McClintock (1983);BSC—Bright Star Catalog (Hoffleit and Jaschek 1982);EXO—EX OS AT Database of optical and other astronomical catalogs;GCV—General Catalog of Variable Stars (Kholopov et al. 1985-1988);HB—Hewitt and Burbidge (1986);HD—Henry Draper Catalog (Cannon and Pickering 1918-1924);MCS—McCook and Sion (1986);MS—Einstein Extended Medium Sensitivity Survey (Gioia et al. 1990);RNG—Revised NGC Catalog (Sulentic and Tifft 1973);WFC—ROSAT Wide Field Camera (Cooke et al. 1991);SAO—SAO Catalog (SAO Staff 1966);SBD—SIMBAD database;SHA—Shara (1990);UGC—Uppsala General Catalogue of Galaxies (Nilsson 1973);VV—Veron-Cetty and Veron (1987);WLY—Woolley Catalog (Woolley et al. 1970); 2;ZCT—CfA Redshift Catalog, Huchra (1990).

Abbreviations for object classification are:AC—active star,AGN—active galactic nucleus,BL—BL Lac object,CG—cluster of galaxies,

2This is an extended version of the Gleise catalog, using the same numbering scheme as Gleise

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CV—cataclysmic variable,GAL—normal galaxy,P—pulsar,S—normal star,SNR—supernova remnant,WD-white dwarf,XRB-X-ray binary,(XRB-Be)—X-ray binary (with Be star secondary).

6.2 Notes On Individual Objects

1ES0013+195: The error box also contains G 32 -7 (S:M4.5), but at V = 14 (cf.13 for G 32 —6) it is an unlikely counterpart based on fx/fopt (Maccacaro et al.1984).

1ES0100+405: The stars G132 -51B and G132 -51C are in the error box and haveacceptable fx/f0 ratios, although both (at V = 13.01) are 2.2 magnitudes fainterthan G 132 -51A.

1ES0120+004: Besides the star, the error box contains MCG +00-04-103, a 16thmagnitude galaxy which may be an AGN.

1ES0122+084A and B: Besides the cluster, the error box also includes the galaxyUGC 977, which may be a previously unknown AGN.

1ES0237-531: The error box also contains SAO 232842 (S:K5), which at V = 8.3is 0.9 magnitudes fainter than HD 16699.

1ES0255+128: Besides the cluster, the error box also contains the galaxy UGC2438, another possible AGN.

1ES0305-284: The error box also contains LTT 1477 (S:M3), but this source hasV = 14.0, and can be ruled out by fx/f0pt arguments.

1ES0315+681: The error box also contains SAO 12702 (S:MO).

1ES0316+413: Besides the cluster, the error box also contains the AGN NGC 1275,a known X-ray source.

1ES0429+130: The error box also contains HD 286839 (S:KO).

1ES0538-019: In addition to HD 37742, the brightest in the field (V = 1.75), thefield also has HD 37743 (S: BOIII; V = 4.2) and BD-02 1338C (V = 10.0).

1ES0702+646: Other than the AGN, the error box contains SAO 14073 (S: GO).

1ES0716—248: The error box contains a substantial portion of the globular cluster

17

N2362, of which HD 57061 is the brightest star (at V = 4.32). There are morethan 30 other possible counterparts, ranging from V = 8.12 to V = 13, with knownspectral types B2—AO.

1ES0924+232: In addition to the galaxy, there are at least 3 other galaxies in theerror box. One of these, 0924+2312, has similar redshift (GAL:0.021) to U5037. Theothers are 1C 0538, MCG +04-22-055, MCG +04-22-059, and MCG +04-22-260.

1ES0953+693: The error box also contains 0953+6917, a B = 13.7 galaxy whichmay have an active nucleus.

1ES1035—268: Error box contains the compact group HCG 048, which includes thegalaxy counterpart.

1ES1101+384: The error box contains two identifications based on the 2E catalog:Mkn 421 (BL), and 51 UMA (S: A3), but the latter is 2.1' from the 1ES position.Mkn 421 is a well known source at high energies (REF) and is clearly the preferredidentification based on an HRI position (from emJine)).

1ES1215+039: The source is a double galaxy.

1ES1254-172: The error box also contains 1254-1711 GAL:0.049), a possible AGN.

1ES1259+289: The error box also contains 1259+2857 (GAL-.0.030), a possibleAGN.

1ES1301-239: Error box also contains A3541 (CG).

1ES1351+695: Error box also includes MCG12.13.24 (AGN: 0.031). With V = 17MCG12.13.24 is a marginally acceptable candidate based on fx/fopt (Maccacaroet al. 1984). Mkn 279 is the preferred identification based on an HRI position (inetn/me).

1ES1503+017: The counterpart, N5486, is part of a galaxy pair with the fainterN5486A (GAL: 0.007).

1ES1507-076: Error box also contains MKN 1394, a possible AGN.

1ES1549+203: There are two acceptable identifications: LB 906 (AGN), and SAO084044 (S: GO), but the latter is 1.6' from the 1ES position.

1ES1602+178: The UGC counterpart is a galaxy pair. In addition, the error boxcontains an NGC pair at z ~ 0.035 and a Zwicky triple at z = 0.038.

1ES1702+457: The error box also contains two galaxies—1702+4544A (G AL:0.061)and 1701+4544B (GAL:0.007).

1ES1704+545: Triple system (with WLY 9584B, F6V; Wool 9584C).

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1ES1706+787: The error box also contains a Zwicky triple (1706+7842), andanother Zwicky galaxy.

1ES1714+574: Error box also includes NGC 6345 (GAL), 2.7' from the 1ESposition.

1ES1731-325: Error box also includes HD 159176 (S:06V+O6V), possibly a memberof the globular cluster.

1ES1753-290: The error box also contains HD 163247 (S:FOV).

1ES1821+643: Error box also includes Kl-16 (WD: DOZl), which had an EXOSATdetection, (1.2' from the 1ES position). However, the PI bin value (= 6) suggeststhat the AGN is the correct identification, since white dwarfs typically have a meanPI bin of 2 (Schachter et a/,1991, in preparation).

1ES1914+092: Error box also includes SAO 124466 (S: FO).

1ES1928+233: Other then the infrared source, the field contains HD 344462 (S:F5)and HD 344461 (S:AO).

1ES2247+106: Other than the cluster, the error box also contains MCG 2-58-21, a16th magnitude galaxy which is possibly an AGN.

1ES2311-430: The error box also contains 2311-4300 (GAL:0.056), with the sameredshift as the cluster, a possible AGN.

7. IDENTIFICATIONS

Identifications of Slew Survey sources with known X-ray sources have playedan important role in producing this catalog (as detailed in §3). Identificationswith other, primarily optical, catalogs are also useful in providing a final checkon the reality of the sources and the accuracy of the derived positions. Allthe identifications with counterparts presented here come from searching 3' fieldscentered on the Slew Survey positions, based on the 95% confidence radius estimatedin Figure 7d. 554 (52%) of the Slew Survey sources are new as X-ray sources, and689 (66%) have been identified with optical catalog sources, including 170 (16%) ofthe new X-ray sources. Few of these are likely to be chance coincidences since a 3'radius search circle gives ~ 5 x 106 independent bins on the sky. Thus, assumingthat all the objects are randomly distributed, for the ~1000 Slew Survey sourcesonly about one in 5000 objects will accidentally associated with a catalog object.Most catalogs contain fewer sources than this, so one chance coincidence or less percatalog is expected. The SAO catalog (with ~100,000 entries) is an exception. Adetailed examination of the identifications and their reliability will be presented ina forthcoming paper (Schachter et al. 1991).

19

In the case of extended objects, especially supernova remnants and clusters ofgalaxies, this technique may fail to identify some objects. A solution to this problemis to increase the search radius systematically while also checking for any duplicatecounterpart identifications. A preliminary analysis suggests that increasing theradius to ~ 5-15' gives ~ 20%-30% more supernova remnant and cluster candidates.

We are presently extending the identification program to handle the extendedsources in more detail, and also to include the IRAS survey (including both thePoint Source Catalog and the Faint Source Catalog), the HST Guide Star SelectionSystem catalog, and the radio 87GB and UT 327 MHz surveys. Optical magnitudesfor candidate identifications in all fields are being obtained from digitizations of thePalomar and UK Schmidt surveys. An on-line data base of identifications will bemaintained at CfA, accessible remotely through the einline system . To allow fordetailed follow-up, we will make available an on-line ascii version of the sourceidentification list, which will be updated periodically. We welcome contributions tothis identification list, which will be referenced in the database.

7.2 New Identified X-ray sources

Table 7 contains a list of the 170 new X-ray sources with optical identi-fications by object class. By a new X-ray source, we mean a Slew Survey sourceundetected in the EXOSAT, pointed IPC (Harris et al. 1991), or HE A O-AS (Remil-lard 1991) catalogs within 3' of the Slew position. Some sources may not be in thesecatalogs, yet be detected in other X-ray missions (e.g., HEAO-A2, Uhuru, ArielV). Therefore, we inspected other comprehensive X-ray source compilations (e.g.,Bradt and McClintock 1983 ; Kowalski et al. 1984). Three (~3%) of the candidatenew identified X-ray sources were eliminated in this manner: the X-ray binaries4U1755-338 and AQL X-l (4U1908+005), and the cluster A2315 (a HEAO-A2source).

The entries in Table 7 are grouped by object type—AGN, galaxies, clusters,white dwarfs, and stars—while the stars are further subdivided as in Table 5 [active,binaries, early type (OBA), late type (> F), unknown type]. The first column givesthe 1ES (First Einstein Slew Survey) name of the object. If the redshift or stellarspectral type is known, it is indicated in column 2. We list in column 3 the commonname of each object, including only a catalog designator such as PG for commoncatalogs, if the coordinate name is the same as in the 1ES name. An asteriskfollowing the object name signifies an uncertain identification (see §6.2). Column 4lists alternate names of the object, if any.

Based on their txfiopt ratios in comparison with the values given for MediumSurvey sources by Maccacaro et a/., we expect that the new 'galaxies' are previouslyunknown active galaxies, primarily Seyfert galaxies.

20

8. PROPERTIES OF THE SLEW SURVEY

The Slew Survey contains 1075 sources, which are concentrated toward theecliptic poles (figure 17). Half of these sources are newly discovered as X-ray sources.This is the largest list of sources from any 'all-sky' x-ray survey to date.

The range of source fluxes complements well that of the Medium Survey(Gioia et al. 1990, figure 1): there are similar numbers of sources in each survey;they each cover about a decade of flux with excellent statistics; and the Slew Surveysources are on average ten times brighter. The uniform selection of the Slew Surveysources by soft x-ray emission will allow the formation of well-defined samples ofmost classes of x-ray emitter: Stars, CVs, AGN, clusters of galaxies, and BL Lacs.

Some regions of the sky have especially favorable coverage. The Cygnus Loophas ~150 s exposure, which produces an image with over 100,000 photons (figure18). Of more general interest is the North Ecliptic Pole region (figure 19) whichhas between 30 and 100 seconds exposure. In the region within 10 degrees of theEcliptic Pole 21 sources can be seen, illustrating the ability of the Slew Survey todetect new 'serendipitous' sources.

Two examples of the uses of the Slew Survey samples are given below, onefor quasars the other for BL Lacs:

(1) The steep luminosity function of AGN means that low luminosity AGN(i.e. Seyfert galaxies) are likely to make up a major part of the AGN contributionto the diffuse x-ray background. Yet most optical studies cannot treat these AGNbecause the host galaxy leads to fuzzy images and dilutes the AGN colors, bothof which effects produce uncertain levels of incompleteness in the samples. ThusSchmidt and Green (1983), for example, could not extend their luminosity functionfainter than Mv = —23. The Slew Survey will give a bright AGN survey, similar tothe Palomar Bright Quasar Survey ( BQS, 'PG', Schmidt and Green 1983), but withthe advantage that it is free from the problem of galaxy starlight contamination.AGN will be seen down to My ~ —20 up to z~0.1, complementing the MediumSurvey which reaches a similar absolute magnitude but has few AGN at z<0.1.The Slew Survey may also be a good means of finding high luminosity quasars ofmoderate redshift since, being rare, they require large sky coverage to be detected.Another problem, the dependence of AGN evolution on the unknown spectrum ofthe sources (Elvis et al. 1986, Tananbaum et al. 1986), can be removed empiricallyby using the Slew/A-2 flux ratios.

(2) There is a peculiar break in the x-ray logN-logSfor BL Lac objects, whichmay be related to relativistic beaming in these sources (Giommi et al. 1991) or tocosmological evolution (Wolter et al. 1991, Morris et al. 1991). The flux regionof the break is not presently well-sampled. This is the range covered by the Slew

21

Survey. Recent x-ray surveys (Stocke et al. 1989) have clearly demonstrated thatx-ray selection is currently the best method of discovering BL Lacertae objects. Forthe flux limit of the IPC Slew Survey a uniform, x-ray selected, sample of ~100objects will be detected (and identified through our ongoing program to identify allSlew Survey sources) in the high Galactic latitude sky. This compares with a totalof 87 BL Lac objects, selected by all methods, in the Hewitt and Burbidge (1987)Catalog. There are about 40 known x-ray selected BL Lacs. All x-ray selectedBL Lacs are radio-loud (Stocke et al. 1989) and have well-defined and distinct x-ray/optical/radio flux ratios (Giommi et a/., 1991). This tight aRo/aox distributionimplies that the BL Lacs in the Slew Survey will have radio flux densities in therange 50-80 mJy. This, when combined with the correlation between radio andoptical fluxes, gives an expected my in the range 18-19 for the faintest objects.The three fluxes alone are sufficient to select a large sample of BL Lac objects forfurther study.

Identification of the unidentified Slew Survey sources should be relativelyeasy since they are all bright. We can estimate their optical magnitudes using thenomogram constructed for Medium Survey sources (Maccacaro et al. 1988). Thetypical AGN will be at V ~ 16m and the faintest M dwarfs will be at ~ 14m.This is 2-3 magnitudes brighter than the the Medium Survey identifications andour error circles have only ~5 times their area, so the typical number of possibleoptical candidates, and possible spurious counterparts, will be few. Many of the newsources will also show up in the IRAS (IRAS 1988) and Green Bank (Condon andBroderick 1989) surveys. We will use the Minnesota POSS (Humphries 1988) andEdinburgh UK Schmidt digitizations to derive the bulk of our optical magnitudes.In this way relatively few new optical observations will be needed to make theremaining identifications.

We have not constructed a logN-logS for the Slew Survey in this paper. Thisobvious step is in practice quite difficult to do properly. The uncertainty on thecount rates in the survey are mostly large, so that the 'Eddington Bias' is large.This is the effect by which sources below the formal flux threshold are detected whilesources above the threshold are missed due to flux measurement errors. A simpleflux threshold thus cannot be readily defined. Since the logN-logS is steep (Gioiaet al. 1991) more sources will enter the survey than will drop out, systematicallydistorting and steepening the observed logN-logS at low fluxes. A proper treatmentrequires detailed simulations of the procedures used to produce the survey sourcelist and we defer this to a later paper.

9. CONCLUSIONS

We have presented a survey of the sky in soft (~0.1-3.5 keV) X-rays

22

containing 1075 sources. New, well-defined, samples of bright X-ray sources canbe derived from this survey for many object types. The survey has a limiting fluxa few times fainter than the largest previous all sky survey in X-rays (HEAO-A1,Wood et a/., 1984) which took place in the ~2-10 keV band, and a factor ~10brighter than the typical sensitivity of the ROSAT survey which covers the 0.1-2keV band.

It is fair to ask what the value of the Slew Survey is in the context of themuch larger and more sensitive ROSAT survey (Trumper 1991). This question hasseveral answers: first the Slew Survey makes available rapidly a large number ofnew bright X-ray sources suitable for follow-up study with ROSAT (and, in a fewyears, with ASTRO-D); second virtually all of the existing faint source X-ray workhas been carried out with IPC-selected sources as part of the Einstein MediumSurvey (Maccacaro et al. 1988, Gioia et al. 1990) and the Deep Survey (Giacconiet al. 1979b, Primini et al. 1991), so that a comparison sample of bright identifiedsources selected with the same instrument can be put to use at once for source countand evolution work, without ambiguities due to different detector characteristics;thirdly a comparison of Slew Survey sources with ROSAT survey sources will allowthe selection of unusual objects having extreme variability and/or extreme spectra;and finally the energy band of the Einstein IPC extends to significantly higherenergies than that of the ROSAT survey, so that it will continue to be valuable (e.g.for the selection of hard X-ray sources) even when the ROSAT survey is published.

The large amplitude variations in exposure on a few arcminute scale in theSlew Survey mean that it is not possible to derive upper limits for arbitrary positionson the sky from the present catalog. We are preparing two methods to allow this- an on-line service will be added to einline (the Einstein On-line Service, Harriset al. 1990); and the original, aspect corrected, slew data is available on a CD-ROM as part of the SAO CD-ROM series of Einstein Data Products (Fabbiano1990). This CD-ROM also allows timing, spectral and structural information to beextracted from the Slew Survey via standard X-ray data reduction packages (e.g.IRAF/PROS, MIDAS).

The Slew Survey presently has only coarsely known completeness as afunction of source flux. A program to derive accurate sky coverage and sourcedetection efficiencies as a function of source flux and extent is being initiated.This will allow the derivation of statistical population properties such as luminosityfunctions from the Slew Survey.

We are pursuing a program of identifications for all Slew Survey sources. Thisis initially based on existing archival data and catalogs in an attempt to minimizethe amount of optical observing needed. A first paper on these identifications isin preparation (Schachter et al. 1991). We shall maintain a data base of these

23

identifications as part of the on-line einline system for general use. We welcomeany contributions to these identifications. The on-line data base will include areference for the source of each identification. We ask that any publication usingthis information reference its source as listed in the on-line system.

We have received many requests for information on sources in the SlewSurvey. As a result we are forming working groups for astronomers interested inpursuing an interest in the active galaxies and quasars, and for the BL Lacs in thesurvey. The aim of these groups is to exchange information and prevent unnecessaryduplication of effort, not to direct anyone's research. Anyone interested in joiningone of these groups or in forming another should send e-mail to the Slew SurveyProject (slew@cfa.harvard.edu, cfa::slew). The Einstein Slew Survey data are partof the Einstein data bank. As such they are part of the NASA Astrophysics DataProgram and are available to all interested parties.

There exists some 50% more slew data in the Einstein data bank than wasused for the present survey. These were originally rejected because it had problemsthat would have complicated this first analysis, primarily long data dropouts thatmake the extrapolation of the gyro aspect solution less certain. Our experience nowsuggests that this problem can be overcome and we hope to include this data inconstructing a second 'definitive' Slew Survey, which should have roughly doublethe number of sources.

ACKNOWLEDGMENTS

We thank John McSweeney and the Einstein data center team for assistancewith data handling; Ron Remillard, Jonathan McDowell, Paolo Giommi, JohnStocke and Nick White for their assistance with the identifications, and JohnStocke for a careful reading of the manuscript. This research has made use ofthe Simbad database, operated at CDS, Strasbourg, France. This research has alsomade use of the NASA/IPAC Extragalactic Database (NED) which is operated bythe Jet Propulsion Laboratory, California Institute of Technology, under contractwith NASA. This work was supported by NASA contract NAS8-30751 (Einstein),and NASA grant NAG5-1201 (ADP).

24

TABLES

Table 1: Einstein Surveys

DeepMediumSlew

Area"2.3780

35,060d

f/L(uPPerC) */*m(lower) no- sources~ 7 x ID'14

~ 5 x ID"12

~ 1 x 10~9

~ 4 x 10-14

~ 2 x 10~13

~ 3 x 10~12

25835

1075

ref.Primini et al 1991Gioia et al. 1990this paper

a. Square degrees (59°).

b. erg cm"2 s"1.c. Defined as the flux below which 90% of the sources lie.

d. Defined by the minimum exposure (1.0s) at which a source was detected.

Table 2: Einstein IPC Slew Survey Properties

Observing timeEffective exposure"Total no. of photonsMean backgroundMin. no. of photons/source

(for mean background)Mean exposureMean limiting count rateMean limiting fluxc

No. sourcesIdentifications'*

0.99 x 106s0.47xl0652.6 x 106

~0.7 photons/source box6

5 (PRand ~ 1 X ID'4)

12 s0.45 ct s-1

14 x 10-12 erg cm~2 s'1

1075Stars: my <7AGN: mv

a. including corrections for vignetting and excluding the 'ribs' regions.

6. 6' x 6' box.c. 0.2-4.0 keV, for a conversion factor of 3.26 x 10~n ergs /count appropriate for an a power law

energy index of 0.5 and a Galactic N# of 2.0 x 1020 atoms cm~2 as used in the Einstein Medium

Survey (Gioia et al. 1984)

d. based on Medium Survey nomogram (Maccacaro et al. 1988).

25

Table 3: Relative value of Einstein instruments for slew surveying

(FOVx% timexQE)0 figure of meritIPCHRISSSFPCS

1800x ~0.5x0.7216x ~0.2x0.19x ~0.15x0.9

<90x ~0.15xO.01

6304.31.20.14

a. FOV= field of view in square arcminutes; %time = fraction of time in focal plane; QE = quantumefficiency.

Table 4: Offsets for each set of gyros (in arcminutes)

gyro gyros in usecombination0

ABCDEG

122233

233454

354666

AX

0.03.2

4.256.06.0

4.75

AY

0.00.0

1.250.0

1.751.75

a. gyro combination F did not contribute usable slews to the survey.

26

Table 5: Identified Sources to Date

Class Num. New Total Num. % Survey % SurveyX-ray Src. IDs. Pet. Pred. (MS)

AGN 10 131 19 30BL Lacs 0 33 5 10Clusters 12 80 11 20CVs 0 23 3 6Stars 121 274 40 20

Known Active 2 48Binaries 4 19Wind Cand. (DBA) 18 38Coronal Cand. (>F) 89 149Unk., Pecul. 8 20

X-ray binaries 0 41 6 6and Pulsars

Other: 27 109 16 8Galaxies 22 42SN Remnants 0 28White Dwarfs 1 62E Sources 0 25SIMBAD Sources 4 6EX OS AT Sources 0 2

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60

Table 7: New Identified X-ray Sources

Name

1ES0702+6461ES0836+7101ES0921+5251ES1149-1101ES1251-2811ES1309+3551ES1320+0841ES1415+4511ES1518+5931ES1626+554

1ES0005+1451ES0205+4921ES0257+4421ES0403-3731ES0412-3821ES0502+6751ES0543-5551ES0559-3991ES0924+2321ES1121-0121ES1141+7991ES1215+0391ES1217-1681ES1234+4591ES1238-3321ES1254-1721ES1318+2741ES1323+7171ES1324-2691ES1324-2681ES1336+2801ES1714+574

1ES0058+3451ES0122+084A1ES0122+084B1ES0644-5411ES0914+5191ES1241+2751ES1256-0391ES1301-2391ES1310-327

Type/z

0.0792.1600.0360.0490.0690.1840.0500.1140.0790.132

** .

...• • •

0.0550.050...

0.015• . .

0.026• . .

...0.075• . .

...

* . *

0.046• • .

0.0720.046* * >

0.0360.028

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0.1970.2410.083• • •

• *.

Counterpart Name Other Counterpart Names

AGNVII ZW 118*4C 71.07 S5 0836+710MKN 110PGESO 443- 5TON 1565 PGMKN 1347PGSBS151S+593PG

Galaxies?Z 0005.5+1433G 173 -39U02468ESO 359- 19ESO(B) 303RZ 0502.3+6735NGC 2087 ESO 159-26GAL 0559-3959UO5037*Z 1121.0-0117UO67284C +04.41* PKS 1214+038MCG-3.32.4Z 1234.5+4556ESO 381- 7GAL 1254-1710*G 149 -80GAL 1323+7145ESO 509- 9ESO 509- 14Z 1336.4+2800NGC 6338* U107S4

Clusters of GalaxiesZW 314A193*A193*A3404A773A1602A1651A1664*S724

61

1ES1900+699 0.0941ES2217-354 ...1ES2247+106 0.0771ES2349-561 ...

1ES1631+781 DA

A2315A3866A2495*Si 158

White DwarfsWFC 1629+781

Stars: Known to be Active1ES0957+247 KOVE+B DH LEO SAO 0811341ES2058+398 M3EV+M3EV VVLY 815AB

1ES0154-518 G5IV+1ES0309-291 F8IV+1ES1314+172 K2V+M2V1ES1833+169 G2V+G2V

1ES0157+7061ES0324+0951ES0426-1311ES0510-1191ES0651-0201ES0839-4451ES1126-6101ES1148-6241ES1225-5511ES1318-6321ES1348-5881ES1414-1971ES1650-4171ES1753-2901ES1920+2231ES2132+2881ES2157+5701ES2235+434

A3IVB9VnBlVneB8VBAOAB8A2BB9IVA5IVBA3A2AOAOA3

1ES0013+195 M41ES0032-622 K5V1ES0048+236 F51ES0054-702 F81ES0120+004 GO1ES0133+484 gKl1ES0143-253 FlV1ES0226-615 F8

Stars: BinariesWLY 81ABWLY 127ABWLY 505ABHD 171746

SAO 23273, X ERI, HD 11937SAO 168373, a FOR, HD 20010SAO 100491SAO 103886

Stars: Early TypeSAO 4554 48 CAS, HD 12111HD 21364 214 TAU, SAO 168373DU ERI HD 28497, SAO 149674SAO 150223 309 LEP, HD 33802HD 292785HD74209HD 306536HD 309207SAO 239967LS 3039SAO 241229SAO 158468SAO 227370HD 163300*HD 344230AG+282503SAO 033950SAO 052191

Stars: Late Type*G 32 -6*HD 3221AG+23 78SAO 255722HD 8358*HD 9746 SAO 037351f SCL HD 10830, SAO 167275SAO 248569

62

1ES0238+0571ES0305-2841ES0308-0551ES0315+6811ES0357-4001ES0415+2311ES0419+1481ES0423+1461ES0424+3261ES0428+3661ES0429+1301ES0444-7041ES0447+0681ES0504-5751ES0603-4841ES0614+2271ES0618-5801ES0635-6981ES0637-6141ES0712-3631ES0717-5721ES0738+6121ES0740+2281ES0919+4041ES0920-1361ES0923-5301ES1002-5591ES1020+4931ES1026+6201ES1101-6061ES1105+8331ES1212-6521ES1212+0781ES1228-4651ES1239-0111ES1252-0601ES1301-4111ES1325-2611ES1325-3121ES1326+7891ES1327-3131ES1339-6881ES1354-3141ES1358-6731ES1414+2031ES1437-2521ES1456-400

MK7VKOFOKOKOF8G7IIIG8G5F8K7F6VF8VG5K2K2VG3VG1-2VF6-7VGOIV-VKOKOK2VKOIVF7VK1-2IIIF5F8MOKOGO/G1VKOF5VFOVK8VKOK5IIIF5VG2.5lIIbK1IIIG2IV-VKOVKill-IllF8VFO/F2VF7/F8V

BD+05 378CD-28 1030*SAO 130323AG+68 165*HD 25300HD 284303HD 285758SAO 093935HD 282099SAO 057285HD 286840*HD270712SAO 112106WLY 189SAO 217708HD254475SAO 234448HD 47875HD48189SAO 197732SAO 235087SAO 014296SAO 079647SAO 042826SAO 155136SAO 236956SAO 237656HD 89944ZZUMASAO 251235SAO 001824HD 106392SAO 119284SAO 223481WLY 482AWLY 9424CD-40 7655HD 117033SAO 204500HD 117566SAO 204527SAO 252423SAO 205032SAO 252570HD 125040HD 129009HD 132349

7316 TAU, HD 28100

WLY 178, 1163 ORI, HD 30652ZETA DOR, HD 33262, SAO 233822HD 41824

SAO 249604

SAO 138917, HD 110379, HD 110380

SAO 007821

SAO 083259

63

1ES1507-0761ES1509+7631ES1519+2111ES1606+2181ES1614+4461ES1702+4571ES1711-5471ES1716+5511ES1727+5901ES1737+6121ES1746+7481ES1753+3621ES1811+0061ES1824+1511ES1853+2341ES1900-4101ES1902-5241ES1914+0921ES1928+2331ES2001+0681ES2005+1601ES2013+4481ES2042+3351ES2048+3141ES2052+4411ES2052-1721ES2128+2311ES2135+0111ES2153+4411ES2216+8451ES2257-3401ES2326+4111ES2334+0631ES2347+361

1ES0406+0991ES0437-0461ES0437+4441ES0829+1591 ESI 735 -2691 ESI 84 1-0441ES2129-0261ES2155-081

KOG5MOEVK2GOF8FOIV-VKOGOMKOG5KOKOK2VG8IIIF7VK2IIM8K2G5KOG5KOG2VF8VK8KOKOK2G5VPM2GOG1IIIE

Stars:.*.

• * •

• *•

..•

...

• • •

• •*

...

SAO 140351*SAO 008175WLY 9520AG+21 1576SAO 045997SAO 046462*SAO 244557SAO 030326SAO 030416HD 160934SAO 008910SAO 066472SAO 123267SAO 103722V775 HER WLY 9638HD 176705p TEL HD 177171SAO 124465*IRC +20412*HD 190342SAO 105730SAO 049357SAO 070451SAO 070569SAO 050198SAO 163989BD+22 4409AG+01 2623SAO 051437SAO 003717SAO 214237G 190 -28SAO 128282SAO 073535 HD 223460

Type UnknownEG 7-114BF ERIOU PERSAO 097895IRAS 17345-2656 ...FT SCTPHL 26BD-08 5773

NOTES—° These galaxies, although catalogued as normal, may possessactive nuclei.

b Many of the late type stars may be previously unknown active stars.

64

REFERENCES

Abell G., 1958, ApJS, 3, 211.Abell G., Corwin , and Olowin, 19S9, ApJS, 70, 1.Bradt, H. V. D., and McClintock, J. E. 1983, ARA&A, 21, 13.Cannon A.J., and Pickering E.G., 1918-1924, The Henry Draper Catalogue, Ann.

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Figure Captions

Figure 1: Distribution of source fluxes from the Slew Survey (solid line)compared with those of the extended Medium Survey (dashed line; Gioia et al.1989) and the Deep Survey (dotted line; Primini et al. 1991)

Figure 2: Exposure map for the Slew Survey in Galactic coordinates. Slewpaths are readily seen going in great circles between the Ecliptic poles.

Figure 3: GX 5-1 (1ES1758-250) seen before (a) and after (b) Slew aspectwas applied. Applying the slew aspect correction, which takes into account themotion of the satellite, produces a well-defined image (b). The background overthe whole 1x1 degree field shown is 65 counts for an exposure of 14 seconds.

Figure 4: Fraction of the sky to a given exposure in the Slew Survey.

Figure 5: Initial offsets in arcminutes between Slew derived and accurate X-ray source positions for 172 known X-ray sources (Remillard et al. 1991; 2ECatalog) detected in individual slews.

Figure 6: (a) Offset in arcminutes (perpendicular to slew direction) betweenthe Slew calculated position at the end of the slew and the accurate positionfrom the pointed, star tracker, solution vs. slew length in degrees. The plotis for the data before the application of the correction made by rotating theassumed plane of the gyro assembly, and is for gyro combination B. The solidcurve shows the size of the correction. (6) Offsets as in (a) after gyro orientationcorrections.

Figure 7: (a) Offsets of Slew source positions from Bright Star Catalogidentifications, in R.A. and Dec., after all aspect corrections are applied.(6) Offsets as in (a) but for an artificial set of Slew Survey sources createdby shifting the real Slew Survey source by one degree in II.A.. This showsthe background rate of identifications due to accidental matches of position,(c) Radial version of (a) with a heavy line marking the false identificationbackground rate from (b) (d). Integrated histogram of (a) with the backgroundfrom (6) subtracted.

Figure 8: Percolation algorithm flowchart.

Figure 9: Four typical regions of the Slew Survey exposure map. Each regionis 30' on a side, the size of background region 2, and is centered on a Slewsource. (The 1ES name is given for each.)

67

Figure 10: Number of candidate sources with 1 photon detected by thepercolation algorithm vs. Poisson probability, PTa.nd- The solid line shows thenumber expected assuming there are no real sources in the data. This is areasonable approximation for three decades of Prand-

Figure 11: Integral histogram of number of candidate sources with greaterthan or equal to 3 photons detected by the percolation algorithm us. Poissonprobability, PTand- The solid line is the number expected if there were no realsources in the data.

Figure 12: Percentage of Total Candidate sources that are false sourcesvs. Poisson probability, Prand- The false source fraction reaches ~2% at ourthreshold of log Prand = -3.95.

Figure 13: Offset in arcminutes between the Slew source positions and theaccurate positions of known X-ray sources (for objects in Remillard et al. 1991and nonextended objects in the 2E catalog) vs. probability of a source arisingby chance.

Figure 14: Fraction of Slew sources lying within 2' of the position of a knownX-ray source (for objects in Remillard et al. 1991 and nonextended objects inthe 2E catalog) us. probability of a source arising by chance.

Figure 15: The M81/M82 region showing how the high density of backgroundphotons confuses the percolation algorithm with the standard percolationradius of 2 arcminutes.

Figure 16: (a) Slew Survey count rate us. ratio of Slew/Pointed IPC count rate('2E'). (b) Slew Survey count rate restricted to PI 2-10 us. ratio of Slew/PointedIPC count rate ('2E').

Figure 17: Distribution of Slew Survey sources in Galactic coordinates. Theconcentration of sources at the Ecliptic poles ('NEP' and 'LMC'), where theSlew Survey exposure time is greatest, is clear.

Figure 18: Slew Survey image of the Cygnus Loop. The mean exposure timein this image is ~150 seconds. 108,000 photons are included in the image. Thefield shown is 4x4 degrees.

Figure 19: The region of the Slew Survey within 10 degrees of the NorthEcliptic Pole. The exposure time ranges from ~100sec (North) to ~30sec(South) which leads to the variations in photon density seen in the image. Theimage is not exposure corrected. The two darkest areas are short segments ofdata from the very beginning or end of slews when the spacecraft is virtuallystationary. The 21 Slew Survey sources are circled. (One source is almosthidden in the heavily exposed region to the lower right.)

68

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