H\alpha emission-line stars in molecular clouds.

H emission-line stars in molecular clouds.

II. The M42 region.
Bertil Pettersson Observational Astronomy, Department of Physics and Astronomy, Uppsala University, Box 516, SE-751 20 Uppsala, Sweden
Bertil.Pettersson@physics.uu.se
   Tina Armond Universidade Federal de Sergipe, Departamento de Física, Av. Marechal Rondon s/n, 49100-000, São Cristóvão, SE, Brazil
tina@ufs.br
   Bo Reipurth Institute for Astronomy and NASA Astrobiology Institute, University of Hawaii at Manoa, 640 North Aohoku Place, Hilo, HI 96720, USA
reipurth@ifa.hawaii.edu
Received 7 February 2014 / Accepted 4 June 2014
Key Words.:
Stars: emission-line – Stars: formation – Stars: pre-main sequence

We present a deep survey of H emission-line stars in the M42 region using wide-field objective prism films. A total of 1699 H emission-line stars were identified, of which 1025 were previously unknown, within an area of 55 55 centred on the Trapezium Cluster. We present H strength estimates, positions, and photometry extracted from 2MASS, and comparisons to previous surveys. The spatial distribution of the bulk of the stars follows the molecular cloud as seen in CO and these stars are likely to belong to the very young population of stars associated with the Orion Nebula Cluster. Additionally, there is a scattered population of H emission-line stars distributed all over the region surveyed, which may consist partly of foreground stars associated with the young NGC 1980 cluster, as well as some foreground and background dMe or Be stars. The present catalogue adds a large number of candidate low-mass young stars belonging to the Orion population, selected independently of their infrared excess or X-ray emission.

1 Introduction

The Orion Molecular Cloud is the nearest giant molecular cloud, a site of intense star formation and one of the most thoroughly studied regions of the sky. The cloud extends for 15 degrees in an elongated shape that can be divided into two subregions, Orion A to the south and Orion B to the north, each having M of molecular gas (Maddalena et al. 1986).

The well-known OB association Orion OB1 extends through the Orion constellation and constitutes subgroups of different ages and locations, sometimes partially superimposed. Associated with the OB stars (Briceño 2008), the region contains a rich population of intermediate and low-mass young stars. Bally (2008) presents an overview of the young stellar populations, and the morphology and possible formation history of the cloud.

The prominent Orion Nebula, M42, is an HII region located in the northern part of the Orion A molecular cloud, corresponding to Lynds 1640. To the south, the cloud extends to Lynds 1641, also part of Orion A.

Menten et al. (2007) estimate a distance of 414 pc to M42, which is the distance we assume here for the entire Orion A cloud.

The M42 nebula is excited by the massive stars of the Orion Nebula Cluster (ONC), mainly by the Trapezium, a tight cluster of massive young stars. The ONC is one of the youngest and most active sites of star formation of the cloud, studied in detail at many wavelengths (e.g. in the optical by Hillenbrand 1997 and Da Rio et al. 2009, in X-rays by Getman et al. 2005, in the near- and mid-infrared by Megeath et al. 2012). An extensive overview of the ONC can be found in Muench et al. (2008) and O’Dell et al. (2008).

Fewer studies extend the coverage to the wider areas outside of the ONC. Carpenter et al. (2001) used 2MASS to identify over a thousand young stars in Orion A through their variability. They examined a 084 6° strip centred on the ONC and found a distribution that correlates with the H emission-line stars and the molecular gas. Most of the variability can be explained by cold and hot starspots, by accretion, or by varying extinction.

Davis et al. (2009) imaged Orion A in H 2.122 m in search of molecular hydrogen outflows and their sources, which they classify as mostly protostellar. The Spitzer survey from Megeath et al. (2012) covers Orion A and B and classify 2991 pre-main-sequence stars with disks and 488 as likely protostars, based on mid-infrared colours that indicate the presence of a dusty envelope or circumstellar material. A catalogue with five mid-infrared colours is presented. They detect variability in 50% of the young sources.

The powerful radiation field and the expanding HII region of the ONC have cleared away some of the cloud surrounding the cluster, making part of the young stellar content visible at optical wavelengths. Such visible young stars are recognisable through the H emission line which is caused by ongoing accretion processes.

Large-scale objective prism surveys focused on the H line have for a long time been an important way to identify young stars in clusters and throughout molecular clouds. In Orion, the pioneering work of Haro (1953) identified 255 H emission-line stars in an area of 3.5 square degrees around the brightest part of M42. Parsamian & Chavira (1982) added additional stars to Haro’s list, following his nomenclature, and listed a total of 534 stars in a 5 square degree region. Additional information on many of these stars is summarised in the catalogues of Herbig & Kameswara Rao (1972) and Herbig & Bell (1988), which were for years a reference for many of the optically visible young stars in Orion.

Subsequently, a large and systematic H emission survey was performed throughout the Orion constellation using the Kiso Schmidt telescope, covering an area of 300 square degrees, resulting in about 1200 emission-line stars detected with limiting magnitude of V=17.5. The results were published in a series of papers, each covering one region in Orion (Wiramihardja et al. 1989; Kogure et al. 1989; Wiramihardja et al. 1991, 1993; Nakano et al. 1995). Their coordinate range in the sky is about , (J2000).

Brand & Wouterloot (1992) present an overview of the low mass star formation in Orion, including a comprehensive list of all H emission-line stars compiled from all the surveys known until then, including their own work in the L1641 cloud (Wouterloot & Brand 1992). The catalogue contains 1297 stars in the range , (J2000). It includes all the Kiso surveys, except for the last two published in 1993 and 1995 (114 stars).

Recently, Szegedi-Elek et al. (2013) performed a survey for H emission-line stars in an area of one square degree around the ONC, using slitless grism spectroscopy. They detected 587 stars with emission, of which 99 are new findings.

Another technique used to detect H emission is through the use of narrow and wide filters centred on the H line. This technique was used by Da Rio et al. (2009). In a 3030 region approximately centred on the ONC they detected 323 stars with a strong line excess exceeding 50 Å in equivalent width and 315 stars with weak H excess corresponding to equivalent widths in the 5 50 Å range. As noted by the authors, the uncertainty in the derived H emission is difficult to evaluate, and may be affected by various problems, including the non-uniformity of the strong nebular H emission. Their survey is mainly focused on the central region of the ONC where we are most affected by the strong nebular background, and hence there is little overlap between our surveys. Finally, one can of course detect H emission by obtaining spectra of individual stars. With modern multi-slit spectrographs this is becoming feasible, as for example demonstrated by the kinematic study of Fűrész et al. (2008), who observed 1215 stars in the ONC, of which 1111 stars were confirmed as members. The disadvantage of this method from the point of view of searching for new young stars is that the targets first need to be selected by some criteria, so the search is not unbiased. In the following, we compare our results only with other objective-prism or grism surveys.

In this paper we continue to present the results of a series of large scale searches for H emission-line stars using photographic films and the large objective prism at the ESO Schmidt telescope, before it ceased operations in 1998. The first of the series (Reipurth et al. 2004, from now on Paper I) studied the NGC 2264 star forming region, where we detected 357 H emission-line stars, of which 244 were new findings. In the present paper we focus on Orion.

The area surveyed here is 55 55 on the sky centred on the Orion Nebula Cluster, covering a wider area than all of the previous surveys except the Kiso survey, but deeper than that one. By going deeper, we are sensitive to lower-mass stars, and also to stars suffering higher extinction.

H emission in young stars is widely assumed to be triggered by accretion from a circumstellar disk through funnel flows onto the star. H emission is thus a measure of a temporary condition, and is therefore expected to be variable, although the timescale of variability is poorly known. An advantage of using H emission to identify young stars is that even stars with little circumstellar material, which are thus difficult to identify as young in infrared surveys, can accrete and produce the tell-tale H emission. H emission-line surveys and infrared surveys therefore to some extent complement each other.

2 Observations

Spectral films (sensitised Kodak 4415) were taken between 1995 and 1997 at the ESO Schmidt telescope at La Silla, equipped with an objective prism that yields a dispersion of 800 Å mm at H, as already described in detail in Paper I. The RG 630 filter used provides a spectral range from 630 nm to 690 nm, a narrow range centred on the H line. Exposure times ranging from 15 minutes to 150 minutes allowed the detection of emission in both faint and bright stars. The very central region of M42, where the nebulosity is too intense, was impossible to examine, even in the shortest exposures. The size of the films (30 cm 30 cm) corresponds to a field of 55 55 on the sky. All exposures were centred on the position : 535 °25′ (J2000). Table 1 lists the films employed in the present study.

Date No. Exp. time Filter Seeing
(minutes) (″)
1995 Nov 24 12093B 120 RG630 1.0
1995 Nov 27 12103B 15 RG630 1.0
1996 Feb 13 12175B 120 RG630 0.9
1996 Nov 20 12852B 40 RG630 0.5
1996 Dec 13 12896B 150 RG630 0.8
1996 Dec 14 12898B 150 RG630 0.7
1997 Jan 06 12935B 40 RG630 0.5
1997 Jan 11 12952B 90 RG630 0.85
1997 Jan 31 12972B 90 RG630 0.8
Table 1: List of Schmidt films

3 The survey

The Schmidt films were visually inspected with the use of a binocular microscope in search of emission against the continuum of the stars. About 2360 candidate H emission-line objects were initially identified. An H strength was assigned to each object, in a range from 1 to 5, following the same procedure used for our NGC 2264 survey (Paper I). The H strength is defined so that 1 is weak emission against a strong continuum and 5 is strong emission against a weak or absent continuum. Only the stars identified as unequivocally possessing emission were retained, and emissions identified as coming from HH objects and some galaxies were also removed, which altogether reduced the number of stars in our survey to 1699.

The POSS-II surveys (from 1987/1988 Digitised Sky Survey, DSS) that provide images with a plate scale of 1″pixel, were used to obtain initial coordinates for the stars. The images were retrieved in FITS format and had astrometric information in their headers. The task MAKEWCS from the IRAF image reducer package was used on each image to add a coordinate system that can be understood by IRAF. The IRAF task IMEXAMINE was used to determine the coordinates of each star visually identified in the finding charts. images were used to measure the coordinates for most of the stars, while images were used in regions where the nebulosity is particularly bright at optical wavelengths.

These initial coordinates were searched (within a radius of 2″) among the stars of the 2 Micron All Sky Survey (2MASS) catalogue in order to obtain near infrared magnitudes. The 2MASS coordinates have expected uncertainties of 01, better than what we achieved with the DSS images. Therefore, the present survey uses the 2MASS coordinates. In some cases with close pairs the 2MASS listed coordinates were not resolved and coordinates were visually measured from 2MASS J frames. Finding charts for the new stars, extracted from the DSS, are presented in Figs. 8-18, available in the electronic version. Emission-line strengths were estimated by eye on each film separately. Differences in estimates are indicated as hyphenated values, and may represent either intrinsic variability and/or uncertainty in the estimate. Nearly 18% of the stars present such differences. The distribution of H emission strength is shown in Fig. 1.

The USNO-B catalogue was used to get blue, red, and infrared photographic magnitudes (, , and ) for most of the stars. Blue and red magnitudes were extracted from the GSC-2.2 catalogue for a few additional stars that were only detected in that catalogue. Both catalogues provide optical magnitudes for about 80% of our stars. We also got crossidentifications with the 2MASS catalogue and were able to obtain near-infrared magnitudes for all but eight stars.

Figure 1: Distribution of H emission strength assigned by eye to the stars. When there was a range of values, the lower one was used.

The brightness distribution of the 1327 H emission-line stars with a (red) magnitude is shown in Fig. 2. The limiting magnitude of our survey is about =17-18 mag. The peak at 16 mag indicates that the vast majority of the stars detected in our survey are low-mass objects, most likely T Tauri stars. The faintest stars either have higher extinction or they are brown dwarfs.

Figure 2: Brightness distribution of the 1327 H emission stars with a magnitude. The limiting magnitude of our survey is about 17-18 mag.

The spatial distribution of the emission-line stars is shown in Fig. 3. The patches that are empty of stars in the central region are located where the nebulosity is too intense, even in the shortest exposures.

Figure 3: Spatial distribution of the 1699 H emission stars in our M42 survey. The patches that are empty of stars in the central region are located where the HII region is very intense, complicating the detection of H emission-line stars. Stars with an H value of 1-2 are plotted with green triangles and 3-5 as red dots. See text for a discussion.
ESOH GCVS KisoHKiso H catalogue from Wiramihardja et al. (1993). HBCHerbig & Bell (1988) catalogue. HaroHaro (1953) catalogue: Haro 4-1 to 4-255, Parsamian & Chavira (1982): Haro 4-256 to 4-495, Haro & Moreno (1953): Haro 5-1 to 5-98. PaCh OtherAn asterisk means a star also listed in Szegedi-Elek et al. (2013) (2000)Positions extracted from the 2MASS All-Sky Catalog. (2000) HThe H strength is defined so 1 is weak emission against a strong continuum and 5 is strong emission against a weak or invisible continuum. Hyphenated values may represent either variability and/or uncertainty in the estimate. A ’+’ indicates resolved spectra but unresolved DSS image. The magnitudes , , and are from the blue (IIIaJ emulsion), red (IIIaF emulsion), and infrared (IV-N emulsion) digitised sky surveys extracted from USNO-B catalogue or from GSC 2.2. magnitudes extracted from the 2MASS All-Sky Catalog. Notes Notes to individual stars.
V731 76-59 4-48 70 05 33 47.71 04 52 08.5 2 16.05 14.54 13.01 11.64 11.03 10.73
76-61 4-99 73 05 33 48.22 05 13 26.2 3 18.36 16.50 14.90 12.99 12.14 11.71
857 * 05 33 48.34 05 22 39.4 1 13.96 12.70 11.99 11.72
858 05 33 48.51 07 13 59.3 2 12.63 18.72 15.83 13.81 13.20 12.91
V354 76-63 4-300 78 05 33 49.54 05 36 20.8 2 15.15 12.37 11.32 10.71
HX 75-186 4-18 75 05 33 50.27 04 38 34.2 3 14.61 13.35 12.30 11.21 10.52 10.29 11
859 * 05 33 50.74 05 00 39.5 2 18.01 16.59 14.91 13.18 12.42 12.12
76-64 4-39 77 05 33 51.35 04 48 22.2 1-2 16.26 14.68 13.64 12.48 11.61 11.27
HY 76-66 4-159 81 05 33 52.36 05 41 50.2 1 15.60 14.52 12.82 11.72 10.90 10.56
860 05 33 52.62 04 57 51.0 3 18.67 16.91 15.43 13.37 12.74 12.46
861 05 33 53.38 07 14 11.6 2 17.58 16.41 13.81 12.88 12.30 12.06 2,8

111 The full table with all the 1699 H emission-line stars is available electronically. A few lines are reproduced here only for guidance regarding format and content.
Table 2: H emission-line stars in M 42

3.1 Comparison with previous surveys

There were 674 stars in our survey that had already been detected in previous objective prism H surveys, yielding a total of 1025 new H emission-line stars in the Orion region. Of the previously known emission-line stars, 436 are found in the compilation from Brand & Wouterloot (1992), which comprises most of the work done until then in surveying the Orion region for H emission-line stars. The star Strom 6 appears in Brand & Wouterloot (1992) but is designated as L1641 N. In addition, 238 stars were found to be in common with the recent survey of Szegedi-Elek et al. (2013). Since the stars of Szegedi-Elek et al. were not given an identifier and their survey was done simultaneously with our present survey, we have retained our ESO-H numbers for those stars that we have in common.

The Herbig & Bell (1988) catalogue (HBC) has 126 stars inside our field, of which we detected 55 (44%). The HBC catalogue was compiled from stars observed with different techniques and at different epochs. At least a dozen HBC stars are located in the brightest M42 area, where our films are overexposed.

Haro’s catalogue (Haro 1953; Parsamian & Chavira 1982) has 530 stars in our field, of which 359 were detected by us (68%). Their coordinates are in some cases rather uncertain, and this plus variability in the line emission must account for the 32% of stars not detected by us.

Among the 471 stars from the Kiso H catalogue of Wiramihardja et al. (1993) that lie inside our field, 314 were also detected by us, a fraction of about 67%. The Kiso catalogue was constructed in a more uniform way, similar to our survey, but the ratio of stars in common is still low. Our survey is much deeper than Kiso’s; our long exposures reach 150 minutes while Kiso’s maximum exposures are 90 minutes, and in the same area surveyed they detected a quarter of the number of emission-line stars detected in our survey. In general the H emission strengths assigned by eye (with the same scale) in both surveys agree very well, but it is noteworthy that most of the stars in common have larger emission strengths, peaking at 3. The undetected Kiso objects were all re-examined on our films; some were located in the overexposed areas, while others were classified by us as possible emitters, but were not included in our final table. About 60% of the undetected Kiso objects certainly show no emission at our resolution.

Figure 4: Distribution of the H emission stars (orange dots) overplotted on a CO map contour from Maddalena et al. (1986).

3.2 Description of the table

A table with the H emission stars in M42 was built using the same criteria as the NGC 2264 survey (Paper I). Some representative lines are listed in Table 2. The full table is available in the electronic version, and will also be available electronically from CDS. The first columns are: the ESO H identification number, assigned only to the stars not detected previously, the variable name or number from General catalogue of variable stars (Kukarkin 1985), followed by the identification numbers of the H emission surveys from Wiramihardja et al. (1993), Herbig & Bell (1988), Haro (1953), Parsamian & Chavira (1982), and other possible names. The coordinates (J2000) are given in the next columns, followed by the H emission strength and the magnitudes obtained in the USNO-B catalogue (, , and ) and in 2MASS (). The last column provides comments on individual objects. Finding charts for individual stars, often located in crowded regions or as components in close binaries, are presented in Figures 8–18, which are available in the electronic version only.

3.3 Spatial distribution and relation to CO clouds

The main concentration of H-emitting stars corresponds very well to the distribution of the gas in the Orion A Cloud, as shown in Fig. 4 in a comparison with a CO map from Maddalena et al. (1986). The region with the largest number of stars matches the area with strongest CO emission, and the stellar density continues to trace the south-eastern L1641 dark cloud. The vast majority of these stars are likely to represent young T Tauri stars with ages approximately similar to the age of the ONC.

Additionally, there is an almost uniform distribution of stars all over the 30 sq. degree area of our survey. This population may have a more complex composition. First, some of the stars may originate in the ONC, and have been scattered away as a result of N-body interactions in the cluster. Second, there is a slightly higher density of H emitters to the west of the cloud, where the extinction is quite a bit lower than to the east. This might indicate that some of the stars could be background stars, for example distant Be stars. Third, and perhaps most important, it is known that there are several generations and populations of young stars in the general direction of the ONC (e.g. Blaauw 1964, Warren & Hesser 1978, and Gomez & Lada 1998). Most recently, Bouy et al. (2014) have argued that there is a rich population in front of the Orion A cloud, centred on and probably originating in the little-studied cluster NGC 1980 just south of the ONC. At an age of 4–5 Myr, this foreground cluster would still have many low-mass members with H emission. We would expect a younger population to have generally stronger emission, whereas an older population would have fewer stars with strong emission. We have examined this, and in Fig. 5 the stellar density of the two groups is plotted as a function of distance to the centre of the ONC. It is evident that the stronger-line stars (H-strength 3,4,5) are indeed more concentrated towards the centre of the ONC, whereas the weaker-line stars (H-strength 1,2) are more distributed. This supports the idea of Bouy et al. (2014) that we are seeing the mixture of two populations of young stars, one related to the ONC and another to the slightly older NGC 1980 region. Additional interlopers from, for example, the NGC 2024 and  Ori regions may be present as well.

Figure 5: Distribution of stellar density with increasing distance to Ori. A difference in distribution between stronger-lined stars (red, dense hatch) and weaker-lined stars (green, sparse hatch) is apparent, with the former more clustered around the Trapezium and a wider distribution of the latter.

It thus appears that the H emission stars found across our field represent two distinct groups, one related to the young population of ONC stars, and another group more uniformly spread across the field with a mixed origin, some coming from the foreground NGC 1980 cluster and others representing scattered ONC stars or background Be stars.

3.4 Near-infrared properties

The H emission stars of our survey that are detected in all three bands of the 2MASS near-infrared catalogue are plotted in a colour-colour diagram () vs. () in Fig. 6. Also plotted are the locations of main-sequence and giant stars from Bessell & Brett (1988) corrected to the 2MASS photometric system (Carpenter et al. 2001), with interstellar reddening vectors from Rieke & Lebofsky (1985).

Figure 6: Near-infrared colour-colour diagram based on 2MASS data showing all the H emitters in M42 with 2MASS detections in all the three bands (), except upper limits. Main-sequence and giant loci from Bessell & Brett (1988), corrected to the 2MASS photometric system (Carpenter et al. 2001) and the extinction law from Rieke & Lebofsky (1985), are represented in the figure. Symbols as defined in Fig. 3.

Of 1664 stars with valid magnitudes, 26151 have infrared excess, one indication of the presence of circumstellar material. The uncertainties in the 2MASS magnitudes are on average 0.04 mag and can raise or lower the number of infrared-excess stars by about a quarter.

The fraction of H emitting stars with infrared excess is only 164%. In our survey of NGC 2264 (Paper I) performed with the same equipment, we found that 238% of the H emitters show an infrared excess, which is similar within the cited errors. There can be several reasons that only a relatively small fraction of H emitters have infrared excess. First, many weak-line T Tauri stars have little circumstellar material. Second, not all H emitting stars are necessarily young, for example dMe stars and Be stars will have H emission, but no infrared excess. Third, although the population of stars from the foreground cluster NGC 1980 is young, at an age of 4–5 Myr there will be many fewer classical T Tauri stars than among the ONC population. Fourth, even young stars with little circumstellar material can from time to time accrete and thus temporarily produce H emission.

A small number of stars (less than 2%) are located in the so-called forbidden region to the left of the main-sequence locus and the reddening vectors, but all of them are faint and/or located in nebulous regions, suggesting that their 2MASS uncertainties are underestimated.

In Fig. 7 the distribution of the stronger-lined stars (H-strength 3,4,5) and the weaker-lined stars (H-strength 1,2) is plotted in a WISE two-colour diagram used to classify young stars into Classes I, II, and III based on infrared excess as an indicator for the presence of circumstellar material (e.g. Koenig et al. 2012). Of the few stars that fall in the Class I category almost all have strong H emission. The Class II category is also dominated by stars with stronger emission, although a sizeable number of weaker-lined stars are also in this category. The Class III category is strongly dominated by stars with weak line-emission. Since H-emission is mainly an indicator for ongoing accretion, these results follow the intuition that stars with more circumstellar material are more likely to be actively accreting.

Figure 7: Distribution in a WISE two-colour diagram, separating stronger-lined stars (red dots) from weaker-lined stars (green triangles). The dashed lines separate Class I, II, and III sources, see discussion in Koenig et al. (2012)

4 Conclusions

We have observed the central Orion region in a deep wide-field survey for H emission-line stars, detecting 1699 stars with emission, of which 1025 were previously not known to show H emission. The stars fall into two groups, one that contains most of the stars and is distributed along the L1641 cloud, and another that is more or less uniformly distributed. A detailed photometric and spectroscopic follow-up study is required to more precisely identify which stars are likely to be members of the young ONC population, or of the slightly less young foreground NGC 1980 population, or are general foreground or background stars.

Acknowledgements.
We are grateful to Guido and Oscar Pizarro, who as telescope operators obtained all the films used in this survey, and to the referee, Hervé Bouy, for a very helpful report. TA acknowledges financial support from CNPq-Brazil under the process number 200279/2009-2. BR acknowledges support through the NASA Astrobiology Institute under Cooperative Agreement No. NNA09DA77A. We acknowledge use of the Digitised Sky Survey and of the SIMBAD database, operated at CDS, Strasbourg, France, and of NASA’s Astrophysics Data System Bibliographic Services. This publication makes use of data products from the Wide-field Infrared Survey Explorer and from the Two Micron All Sky Survey.
\onlfig
Figure 8: Finding charts, 90″ to a side. North is up and east to the left.
Figure 9: Finding charts, 90″ to a side. North is up and east to the left.
Figure 10: Finding charts, 90″ to a side. North is up and east to the left.
Figure 11: Finding charts, 90″ to a side. North is up and east to the left.
Figure 12: Finding charts, 90″ to a side. North is up and east to the left.
Figure 13: Finding charts, 90″ to a side. North is up and east to the left.
Figure 14: Finding charts, 90″ to a side. North is up and east to the left.
Figure 15: Finding charts, 90″ to a side. North is up and east to the left.
Figure 16: Finding charts, 90″ to a side. North is up and east to the left.
Figure 17: Finding charts, 90″ to a side. North is up and east to the left.
Figure 18: Finding charts, 90″ to a side. North is up and east to the left.

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\onllongtab
ESOH GCVS KisoHKiso H catalogue from Wiramihardja et al. (1993) HBCHerbig & Bell (1988) catalogue. HaroHaro (1953) catalogue: Haro 4-1 to 4-255, Parsamian & Chavira (1982): Haro4-256 to 4-495, Haro & Moreno (1953): Haro5-1 to 5-98. PaCh OtherAn asterisk means a star also listed in Szegedi-Elek et al. (2013) (2000)Positions extracted from the 2MASS All-Sky Catalog. (2000) HThe H strength is defined so 1 is weak emission against a strong continuum and 5 is strong emission against a weak or invisible continuum. Hyphenated values may represent either variability and/or uncertainty in the estimate. A ’+’ indicates resolved spectra in unresolved DSS image The magnitudes , , and are from the blue (IIIaJ emulsion), red (IIIaF emulsion), and infrared (IV-N emulsion) digitised sky survey, extracted from USNO-B catalogue or from GSC 2.2. magnitudes extracted from the 2MASS All-Sky Catalogue. Notes Notes to individual stars:
1 - Double with 591. 2 - Unresolved photometry. 3 - Double with 590. 4 - 3″ S of Kiso 75-87. Photometry from SDSS. 5 - W component of close pair. 6 - Unresolved binary 608W and 608E. H emission seen in both components, strength 2 and 3, resp. 7 - Unresolved binary 640W and 640E. H emission seen in both components, strength 4 and 1, resp. 8 - NE component of close pair. 9 - W component of unresolved pair. 10 - In small nebulosity.
11 - E component of close pair. 12 - Binary, emission in W, fainter component. 13 - SE component of close pair. 14 - Photometry includes faint component to W. 15 - Double with Kiso 76-91. 16 - Double with PaCh 115. 17 - This object is not V750 Ori. Misidentified in the Simbad database. 18 - Double with 989. 19 - Double with 988. 20 - Chanal’s object.
21 - Double with 1018. photometry in common. 22 - Double with Kiso 76-114. photometry in common. 23 - in common with Kiso 76-118. 24 - in common with 1058. 25 - NW component of close pair. 26 - Double with 1072. 27 - Double with Kiso 76-124. 28 - I from Jones & Walker (1988). 29 - Stellar. 30 - Unresolved double.
31 - SW component of close pair. 32 - Close to 1233. 33 - Close to Kiso 76-162. 34 - Very faint continuum, no photometry. 35 - unresolved from 1238. 36 - unresolved from 1236. 37 - 13 NW of V417 Ori. 38 - Photometry unresolved from 1239. 39 - photometry unresolved. 40 - Double with Haro 4-164.
41 - Double with 1251. 42 - Double with Kiso 76-188. 43 - Double with 1301. 44 - Double with 1411. 45 - Double with 1410. 46 - Double with Kiso 76-231. 47 - Double with 1412. 48 - Photometry contaminated by faint component to SE. 49 - SW component of binary AX Ori. 50 - NE component of brighter AX Ori.
51 - Double with Kiso 76-243. 52 - Double with 1444. 53 - Double with 1467. 54 - Double with 1464. 55 - In L1641 N. 56 - Cohen-Schwartz’s star. 57 - NW of and near brighter PR Ori. No photometry. 58 - Double with 1538. 59 - NW comp to V846. 60 - Double with 1645.
61 - Double with Haro 4-439. 62 - Sugano’s star, Abastumani 24. 63 - Has a faint comp to NW. 64 - On rim of HH 449. 65 - In nebulosity. 66 - Also given as Haro 4-461 by Parsamian & Chavira (1982). 67 - Double with Kiso 76-368. 68 - Double with 1725. 69 - has IR comp to SW.
576 05 24 45.32 04 03 40.3 1-2 18.65 16.94 14.90 13.49 12.84 12.56
577 05 24 49.82 03 59 02.4 1 18.86 16.83 14.75 13.66 12.98 12.73
578 05 25 04.40 06 50 16.1 2 15.93 14.26 12.94 11.93 11.26 11.04
579 05 25 06.06 06 50 03.4 2 18.82 17.01 14.92 13.75 13.08 12.84
580 05 25 19.24 07 21 33.3 3 18.87 16.84 14.55 13.40 12.74 12.45
581 05 25 20.61 06 05 06.1 4 18.48 16.91 14.80 13.19 12.55 12.20
582 05 25 20.93 05 19 30.3 1 17.64 16.24 14.14 12.82 12.21 11.94
583 05 25 26.16 03 43 30.9 2-3 18.79 16.87 14.62 13.32 12.66 12.37
584 05 25 29.75 02 41 11.1 2 17.20 15.21 12.75 12.08 11.83
585 05 25 30.10 03 45 46.7 3 20.09 17.54 15.60 13.85 13.29 12.97
586 05 25 32.10 06 04 38.6 1-2 18.74 16.73 14.64 13.25 12.68 12.43
587 05 25 32.35 07 37 56.0 3 18.28 16.61 14.65 13.52 12.85 12.57
588 05 25 34.47 06 59 00.6 1-2 18.43 16.79 14.41 13.28 12.63 12.39
589 05 25 34.85 07 33 01.5 2-3 19.18 17.35 15.41 14.08 13.45 13.15
590 05 25 35.96 02 54 48.9 3 17.51 15.95 13.77 13.45 12.95 12.57 1, 2
591 05 25 36.10 02 54 48.0 2 17.51 15.95 13.77 13.45 12.95 12.57 2, 3
592 05 25 39.11 03 52 59.9 2 17.81 16.06 14.21 13.26 12.61 12.34
75-86 05 25 39.80 04 11 02.0 4 16.33 14.67 13.51 12.44 11.69 11.14
593 05 25 40.69 05 52 51.3 4 16.47 15.52 4
594 05 25 43.39 07 11 10.6 1-2 19.44 17.19 15.32 14.01 13.34 13.11
595 05 25 46.52 04 22 45.8 2 19.04 16.90 15.11 13.83 13.20 12.94
596 05 25 50.64 07 38 26.3 2 19.00 17.10 14.92 13.77 13.19 12.87
597 05 25 57.68 06 05 07.3 2 18.27 16.27 14.18 13.04 12.42 12.16
598 05 25 57.90 04 47 53.4 4 14.40 13.89 13.57
599 05 25 57.95 06 55 49.4 1 17.94 16.10 14.35 13.39 12.75 12.49
600 05 26 01.51 04 18 29.1 4 20.02 17.64 15.62 14.00 13.40 13.05
601 05 26 01.66 02 39 25.3 1 16.82 15.54 13.36 12.55 11.96 11.70
602 05 26 03.53 06 55 08.4 2 17.64 15.70 13.66 12.48 11.82 11.57
603 05 26 25.72 05 28 50.4 3 19.47 17.35 14.92 14.34 13.69 13.42 5
604 05 26 27.92 04 20 53.2 2 18.94 16.99 14.61 13.27 12.63 12.36
605 05 26 36.72 05 44 25.8 2-3 16.25 14.49 12.99 11.95 11.26 11.06
606 05 26 38.10 04 21 47.5 2 17.82 16.34 14.46 13.37 12.68 12.45
607 05 26 42.40 03 26 47.5 2 19.47 17.31 15.24 13.65 13.02 12.69
608W+E 05 26 53.11 05 59 05.6 2+3 17.30 15.41 13.28 12.42 11.75 11.42 6
609 05 26 55.38 03 00 37.9 2 19.09 17.20 14.62 13.28 12.73 12.40
610 05 26 58.65 03 57 42.8 3 21.03 18.88 17.11 14.89 14.44 14.04
611 05 27 01.01 06 01 10.1 2-3 19.21 16.72 15.17 13.73 13.13 12.89
612 05 27 03.38 02 44 14.9 2 18.42 16.69 14.74 13.49 12.90 12.59
613 05 27 03.96 03 01 41.1 2 20.17 17.29 15.20 13.77 13.10 12.82
614 05 27 10.11 07 59 11.4 2 18.82 16.96 14.95 13.75 13.11 12.91
75-104 4-257 2 05 27 12.17 06 59 54.9 3-4 17.14 15.68 13.79 12.65 11.84 11.33
615 05 27 14.69 05 16 30.1 3 16.46 15.89 14.04 12.72 11.77 11.03
616 05 27 19.20 07 50 42.4 1 19.17 17.26 15.18 13.70 13.12 12.83
617 05 27 27.22 02 55 13.2 3 18.85 16.80 14.84 13.53 12.92 12.59
618 05 27 28.76 03 36 49.4 1-2 18.93 16.90 15.26 14.13 13.49 13.26
619 05 27 36.89 04 10 49.4 1 19.00 17.18 14.56 13.43 12.82 12.51
620 05 27 38.39 04 57 03.0 3 19.26 17.29 15.46 14.08 13.44 13.21
621 05 27 40.94 06 27 00.7 3-4 21.31 18.41 17.40 14.55 14.01 13.70
622 05 27 42.17 06 26 57.7 3 18.97 16.87 14.54 12.94 12.34 12.08
623 05 27 42.87 04 06 52.6 2 19.52 17.40 15.76 14.56 13.91 13.69
624 05 27 43.73 05 00 57.0 2 19.41 17.17 15.27 13.88 13.30 13.03
625 05 27 43.85 04 05 23.0 1-2 17.69 16.13 13.91 12.70 12.03 11.76
626 05 27 45.01 07 19 22.4 2 17.99 16.14 13.77 12.98 12.36 12.08
627 05 27 45.63 03 35 47.3 2 18.06 16.38 14.35 12.91 12.31 12.06
628 05 27 47.38 07 51 48.8 3 19.41 17.62 15.35 13.84 13.24 12.96
629 05 27 47.60 06 50 09.8 2-3 17.43 16.00 13.97 12.85 12.19 11.95
75-111 4-258 3 05 27 48.22 05 16 33.1 2-3 14.46 12.90 12.01 11.23 10.49 10.11
630 05 27 54.29 03 26 54.1 2 16.84 15.14 13.16 12.35 11.61 11.37
631 05 27 56.90 05 05 39.1 3 19.01 17.08 14.86 13.52 12.94 12.65
632 05 27 57.90 05 40 01.1 2-3 18.66 16.60 14.46 12.99 12.50 12.15
633 05 27 59.93 02 43 59.2 2 20.51 17.96 16.37 14.74 14.21 13.98
634 05 28 01.38 06 53 35.6 2 18.13 16.22 14.63 13.46 12.76 12.52
635 05 28 11.79 03 13 47.4 2 17.44 15.81 13.94 13.12 12.39 12.20
636 05 28 13.20 03 45 52.6 1 17.82 16.01 14.12 13.14 12.53 12.27
637 05 28 16.49 03 05 43.6 1 17.64 16.03 13.97 12.89 12.22 11.98
75-114 4-260 5 05 28 17.17 07 37 05.4 3 15.74 14.15 12.50 11.56 10.66 10.12
638 05 28 17.58 03 22 51.1 1 16.41 14.74 13.10 12.07 11.37 11.15
639 05 28 19.36 04 10 09.7 2 18.17 16.34 14.31 13.03 12.36 12.12
4-261 6 05 28 19.42 07 36 26.3 2 14.19 13.00 11.89 11.21 10.52 10.21
640W+E 05 28 20.08 04 52 03.0 4+1 18.89 17.28 15.50 14.92 14.29 13.89 7
641 05 28 21.47 06 00 07.9 2 17.43 16.26 14.59 13.31 12.73 12.37
642 05 28 21.99 05 58 30.0 3-4 18.21 16.37 14.60 13.40 12.77 12.40
75-115 4-259 4 05 28 22.04 06 25 56.0 4 14.88 13.88 14.02 11.63 10.76 10.29
643 05 28 23.50 03 35 58.3 2 17.45 15.45 14.29 13.36 12.71 12.47
644 05 28 28.09 03 23 56.4 3 18.86 17.14 15.34 14.06 13.43 13.20
645 05 28 34.20 02 45 57.9 3 19.65 17.96 15.74 13.99 13.38 13.03
646 05 28 37.33 07 37 55.8 3 18.52 16.79 14.63 13.22 12.60 12.30
647 05 28 40.77 03 54 51.9 2-3 18.93 17.05 15.30 13.81 13.18 12.89
648 05 28 41.11 07 17 38.9 4 17.76 16.59 15.53 13.85 13.22 12.70
649 05 28 54.82 04 51 48.3 2 19.08 17.23 15.03 13.52 12.90 12.62
650 05 28 54.95 03 23 32.4 1 18.17 16.48 14.64 13.55 12.92 12.60
651 05 28 56.50 06 05 16.6 2 18.11 16.45 14.39 13.10 12.47 12.22
652 05 28 59.08 04 52 57.8 1 20.24 17.71 15.85 14.32 13.70 13.47
653 05 29 02.39 03 03 15.3 2 18.32 16.70 14.41 13.28 12.64 12.37
654 05 29 07.75 06 10 08.0 1 17.43 15.88 14.23 13.05 12.40 12.16
655 05 29 08.59 06 35 06.2 2 18.26 16.63 14.77 13.62 12.99 12.66
656 05 29 10.37 07 42 24.9 2 14.64 13.64 12.08 12.77 12.00 11.76 8
657 05 29 15.35 03 30 51.7 3 16.20 15.36 14.37 12.54 11.57 11.06
658 05 29 15.55 03 17 34.8 1 17.72 16.06 14.03 12.74 12.13 11.88
659 05 29 15.58 07 41 01.2 1 18.82 17.14 15.18 13.83 13.17 12.93
660 05 29 16.46 03 25 44.5 2 18.74 16.54 14.88 13.49 12.86 12.59
661 05 29 18.22 04 57 34.9 1-2 17.70 15.72 14.19 12.96 12.10 11.78
662 05 29 18.53 03 07 46.5 1 18.82 16.87 14.74 13.47 12.88 12.60
663 05 29 19.02 02 41 47.2 2 19.85 17.57 15.63 14.16 13.49 13.28
664 05 29 19.21 03 53 47.2 2 20.53 17.71 15.73 13.83 13.26 12.89
665 05 29 20.02 04 19 00.1 3 20.36 18.01 16.04 14.43 13.80 13.51
666 05 29 21.01 04 22 23.0 1 18.97 16.89 14.85 13.49 12.92 12.63
667 05 29 22.21 07 23 48.8 2 17.33 14.86 12.37 11.71 11.40
668 05 29 23.36 04 30 56.4 4 14.53 12.90 11.58 10.81 10.06 9.77 9
669 05 29 24.53 07 22 21.9 1-2 17.72 16.14 14.10 13.07 12.38 12.17
670 05 29 24.68 07 17 50.4 2 17.67 16.39 14.53 13.51 12.83 12.59
75-125 4-264 10 05 29 28.49 07 46 37.0 4 17.43 16.89 15.32 13.85 12.77 11.88
671 05 29 30.61 03 30 06.4 2 18.89 16.83 14.79 13.60 13.00 12.71
672 05 29 30.69 07 01 53.8 2 17.78 16.10 13.90 13.04 12.41 12.16
673 05 29 30.75 06 52 21.2 2 18.64 16.80 14.74 13.36 12.79 12.49
674 05 29 31.69 05 31 51.5 2-3 17.45 15.63 13.86 12.79 12.18 11.96
675 05 29 32.39 07 47 45.7 1 18.43 16.73 14.65 13.46 12.80 12.55
676 05 29 35.83 06 29 22.9 3 16.44 14.42 12.06 11.48 10.48 9.82
677 05 29 35.97 03 20 29.3 2-3 19.47 17.54 15.76 14.24 13.53 13.27
678 05 29 47.94 04 31 18.2 2 18.74 16.77 15.15 14.08 13.46 13.24
679 05 29 48.37 07 30 17.3 2 17.06 15.47 14.03 12.42 11.74 11.49
680 05 29 52.09 05 40 43.7 2 18.78 16.88 15.15 13.45 12.86 12.56
681 05 29 52.78 03 33 39.2 1 15.96 14.11 13.54 13.22
682 05 29 53.26 05 38 15.4 3 19.41 17.33 15.90 14.59 14.01 13.64
683 05 29 56.34 07 57 44.4 5 20.93 19.09 17.60 15.30 14.71 14.37
684 05 30 01.13 06 19 15.0 1-2 18.57 16.58 14.93 13.29 12.69 12.44
685 05 30 04.33 06 38 14.5 1-2 17.32 15.87 13.95 12.67 12.02 11.78
686 05 30 06.35 04 26 55.0 2 18.59 16.08 14.64 13.36 12.81 12.54
687 05 30 10.10 06 00 42.7 2 19.20 17.36 15.84 14.23 13.67 13.45
688 05 30 15.76 06 56 39.3 2 18.85 16.86 15.98 14.71 14.21 14.02
689 05 30 17.29 04 18 10.5 1 19.43 16.84 15.80 14.10 13.50 13.24
690 05 30 19.96 04 12 56.5 2 19.11 16.90 15.31 13.75 13.15 12.89
691 05 30 25.17 06 51 24.6 2 18.59 16.36 15.16 13.42 12.84 12.55
692 05 30 26.13 06 56 59.7 2-3 18.98 17.17 15.54 13.65 13.03 12.74
693 05 30 27.87 07 03 47.4 3 20.14 17.78 16.25 14.06 13.48 13.19
694 05 30 29.02 03 56 42.9 4 18.89 17.52 16.74 14.72 14.10 13.60
695 05 30 31.42 06 25 35.5 1 18.39 16.31 15.02 13.21 12.53 12.32
696 05 30 33.52 02 51 28.2 1 19.01 16.92 15.28 13.48 12.97 12.67
697 05 30 35.59 04 05 01.5 2 18.61 16.80 15.23 13.57 12.91 12.67
698 05 30 36.60 04 37 38.5 1 19.04 16.71 15.35 13.60 12.95 12.70
699 05 30 36.74 02 51 30.9 1 19.50 17.26 15.49 13.67 13.12 12.83
V538 75-137 13 05 30 38.41 05 25 43.6 3 15.57 14.40 13.57 12.09 11.40 11.10
700 05 30 41.65 04 53 54.7 1 16.48 15.14 13.67 13.02 12.77
75-139 05 30 41.83 06 34 33.1 2 17.46 15.51 13.83 11.86 11.14 10.89
701 05 30 42.11 06 26 03.5 4 19.19 16.94 16.01 14.30 13.69 13.36
702 05 30 42.64 04 56 27.4 2 17.07 15.49 13.57 12.20 11.54 11.31
703 05 30 43.11 04 15 54.3 4 20.52 18.12 17.54 14.86 13.87 13.34
704 05 30 44.16 05 20 25.4 2 18.07 16.03 14.71 13.13 12.51 12.22
705 05 30 45.50 07 30 15.5 2 17.68 16.82 17.33 16.41 15.96
75-140 4-267 14 05 30 45.97 07 24 58.1 3-4 17.45 15.69 14.55 12.82 12.04 11.70
706 05 30 55.86 07 22 06.7 1 18.84 17.00 15.42 13.43 12.86 12.56
707 05 31 01.31 05 00 45.6 1 18.94 17.17 15.68 13.94 13.33 13.11
708 05 31 06.39 03 22 31.7 1 16.47 14.57 13.23 12.17 11.47 11.28
75-142 4-269 16 05 31 09.40 06 52 16.7 3 14.55 13.77 12.47 12.07 11.26 10.86
709 05 31 12.75 03 12 11.0 1 18.83 17.44 15.99 14.23 13.60 13.34
710 05 31 22.33 04 59 27.6 1-2 18.40 16.49 15.06 13.42 12.82 12.57
711 05 31 23.26 04 37 19.7 3 18.96 16.76 15.22 13.72 13.05 12.78
712 05 31 24.10 06 43 05.5 1-2 13.35 12.70 12.44
713 05 31 25.13 04 37 58.7 3 20.09 17.56 15.91 13.80 13.21 12.89
75-145 05 31 27.09 04 27 59.4 3 17.51 14.96 14.54 13.08 11.09 9.43
714 05 31 30.09 06 38 58.3 3 17.48 15.67 14.84 13.39 12.42 11.84
715 05 31 30.97 06 15 14.4 4 17.95 15.83 16.14 14.32 13.68 13.22
716 05 31 31.02 03 12 31.8 2-3 20.90 18.44 17.21 14.84 14.17 13.76
75-146 4-270 17 05 31 31.05 06 08 41.7 4 16.56 15.52 14.70 12.86 12.03 11.49
717 05 31 31.39 07 28 04.1 4 20.95 18.34 16.26 14.41 13.81 13.44
718 05 31 35.58 02 51 12.1 1 19.36 16.99 15.70 14.05 13.40 13.13
719 05 31 38.41 03 39 44.9 2 20.05 17.69 16.39 14.67 14.06 13.79
720 05 31 46.64 07 16 30.2 2 15.68 14.42 13.57 12.12 11.39 11.05
721 05 31 50.30 03 03 55.8 1 17.94 16.15 14.64 13.17 12.50 12.26
722 05 31 51.71 05 23 08.2 3 18.45 14.39 13.69 12.01 10.49 9.71 10
723 05 31 51.91 05 41 59.6 2 17.49 15.53 14.19 12.81 12.10 11.76
724 05 31 54.34 03 13 35.2 4 18.66 17.27 15.38 13.31 12.65 12.18
725 05 31 55.06 04 22 53.0 3 17.83 15.90 14.11 12.44 11.85 11.55
76-9 05 31 58.24 04 06 41.7 4 18.87 17.30 15.73 13.84 13.12 12.69
726 05 31 58.34 04 26 20.8 1-2 18.80 16.82 15.38 13.48 12.90 12.60
727 05 31 58.80 05 56 40.6 2 18.01 16.10 14.65 12.89 12.27 12.00
728 05 32 00.92 07 45 17.1 1-2 19.00 16.91 14.54 12.87 12.15 11.91
729 05 32 01.29 05 32 00.6 1 19.59 17.10 16.10 14.23 13.65 13.30
730 05 32 01.92 04 53 54.8 3 17.97 16.03 14.70 13.13 12.45 12.27
731 05 32 02.33 05 23 37.3 3 13.75 13.30 12.63 12.39
732 05 32 04.56 07 47 56.9 1 21.16 18.48 15.44 13.65 13.01 12.78
733 05 32 04.92 05 37 43.1 1-2 18.59 16.82 15.71 13.94 13.33 13.11
734 05 32 05.22 05 30 04.6 1 19.46 17.34 16.04 14.14 13.48 13.33
735 05 32 05.29 06 51 53.1 3 17.64 16.03 14.19 12.50 11.93 11.65
736 05 32 05.60 04 56 08.3 4-5 20.69 18.63 16.83 14.57 14.04 13.67
737 05 32 05.96 03 01 15.9 1 16.33 14.49 12.40 10.58 9.99 9.69
V695 76-10 19 05 32 06.22 04 56 09.9 3 16.95 15.14 14.00 12.71 12.01 11.73
738 05 32 06.59 06 58 07.4 1 18.17 16.36 14.63 12.97 12.36 12.10
V540 75-154 4-277 25 05 32 07.78 06 55 36.8 3 15.44 14.73 14.13 12.46 11.53 11.03
HP 75-153 4-273 21 05 32 08.95 05 02 31.9 1 16.20 14.36 12.99 11.41 10.64 10.40
739 05 32 09.19 04 38 11.7 1 18.39 16.51 15.62 14.32 13.66 13.45
740 05 32 10.00 07 27 30.2 3 18.47 17.51 17.45 16.03 15.25 14.29
741 05 32 10.80 04 55 36.0 1 17.24 15.58 14.58 13.13 12.42 12.20
75-156 4-274 22 05 32 10.80 05 19 35.1 3 16.66 15.22 14.10 12.63 11.96 11.70
76-15 05 32 11.41 05 37 44.1 3 20.08 15.83 15.13 13.12 12.02 11.30
742 05 32 11.93 04 43 16.2 2 19.57 17.46 16.01 14.16 13.56 13.37
743 05 32 12.63 06 12 34.6 1-2 19.86 17.30 15.90 13.96 13.35 13.10
744 05 32 12.89 03 15 14.8 1 16.70 14.93 13.75 12.47 11.72 11.55
75-158 4-278 26 05 32 14.84 06 20 54.8 4 16.20 14.68 13.56 12.43 11.78 11.50
75-157 05 32 15.13 05 35 00.4 1-2 15.77 14.43 13.15 11.75 11.06 10.66
76-19 4-279 27 05 32 18.75 05 13 39.0 4 17.74 15.89 14.99 13.20 12.39 11.80
75-159 4-282 30 05 32 19.87 05 36 54.1 3-4 16.93 15.04 13.91 12.25 11.26 10.84
745 05 32 23.93 04 18 50.9 1 18.50 17.18 15.38 13.54 12.91 12.62
75-160 05 32 24.02 05 05 23.6 2 15.63 13.59 12.23 10.84 9.96 9.56
746 05 32 24.54 05 03 17.1 3 19.68 17.00 15.57 13.63 13.06 12.81
75-163 4-281 29 05 32 24.99 07 40 51.3 3 17.17 15.53 13.32 12.01 11.32 11.14
747 05 32 25.01 05 10 14.4 3 19.43 17.19 15.45 13.57 12.99 12.69
748 05 32 25.11 03 08 49.7 4 18.58 16.94 15.19 13.27 12.67 12.31
749 05 32 25.17 04 37 04.9 3 18.66 17.15 15.42 13.48 12.89 12.54
75-161 4-280 28 05 32 25.67 03 43 13.7 3 15.16 13.47 12.99 12.03 11.28 10.94
750 05 32 25.68 04 38 58.4 2 19.10 17.16 15.55 13.66 13.13 12.80
751 05 32 25.82 07 17 29.6 2 16.71 17.03 15.14 13.20 12.57 12.34
752 05 32 26.87 05 16 06.7 4-5 19.80 17.48 17.26 14.65 13.96 13.41
753 05 32 31.17 05 10 58.1 4 20.32 17.34 16.25 13.99 13.45 13.17 11
754 05 32 31.58 03 11 43.5 3 18.01 16.13 14.64 13.12 12.48 12.14
75-165 4-284 32 05 32 33.00 06 08 53.9 4 19.82 17.07 15.96 13.98 13.39 13.07
755 05 32 34.03 05 14 15.8 1-2 18.31 16.46 14.79 13.24 12.62 12.38
756 05 32 35.13 05 37 17.2 1 19.98 17.51 15.30 12.96 12.11 11.70
757 05 32 36.62 04 41 36.4 3 17.91 16.04 14.88 13.13 12.42 12.02
758 05 32 36.76 05 06 15.1 3-4 20.13 17.52 15.81 14.04 13.40 13.11
759 05 32 36.77 06 45 18.3 2-3 16.78 15.29 14.06 12.56 11.86 11.66
76-28 05 32 48.47 04 41 43.5 1 12.65 11.94 11.73
760 05 32 41.70 05 05 53.7 1 18.42 16.87 15.49 14.18 13.56 13.37
761 05 32 42.55 06 01 25.8 1-2 18.32 16.18 14.99 13.40 12.77 12.53
762 05 32 42.94 06 36 38.4 2 17.49 16.04 14.22 12.76 12.11 11.81
763 05 32 42.99 02 58 27.3 3 20.42 18.22 16.25 13.87 13.15 12.86
764 05 32 43.07 03 34 07.3 3 17.76 13.34 12.71 12.44
75-168 4-145 33 05 32 43.42 05 35 57.2 4 16.83 14.42 13.13 11.89 10.90 10.41
765 05 32 44.54 05 24 15.2 3 19.93 17.68 16.37 14.31 13.65 13.27
75-170 4-285 34 05 32 44.65 05 53 24.1 1 16.90 15.22 14.23 12.89 12.27 12.06
766 05 32 44.89 06 34 09.0 3 18.44 16.84 15.07 13.10 12.50 12.23
75-171 4-286 35 05 32 45.33 05 38 14.9 1-2 16.58 14.60 13.45 11.81 11.00 10.68
767 05 32 45.74 04 12 13.4 4-5 19.86 18.15 15.63 15.17 14.80
UZ 76-29 4-155 36 05 32 47.32 05 39 42.7 3 16.18 15.58 13.61 12.36 11.63 11.43
768 05 32 47.92 04 40 49.9 1-2 18.68 16.33 15.34 13.43 12.84 12.59
769 05 32 48.82 05 30 54.3 3 21.54 18.54 16.89 14.03 12.62 11.72
4-287 37 05 32 49.93 06 10 45.6 4 18.67 16.92 15.84 14.11 13.45 13.15
770 05 32 50.25 04 26 35.0 2 18.53 16.54 14.96 13.49 12.84 12.62
771 05 32 50.30 06 45 24.2 1-2 17.81 16.15 14.27 12.83 12.26 11.97
772 05 32 50.53 05 36 12.0 1-2 18.70 16.68 15.23 13.66 13.11 12.90
773 05 32 50.88 07 29 07.7 2 20.36 18.10 15.14 13.24 12.63 12.32
774 05 32 51.26 03 40 36.4 3 18.82 16.85 15.42 13.47 12.87 12.51
775 05 32 51.87 07 40 30.0 2 19.90 18.01 16.38 14.65 13.96 13.71
776 05 32 52.39 06 50 22.1 2 18.43 16.68 14.87 13.15 12.52 12.30
777 05 32 52.57 04 11 43.7 2 20.06 17.63 16.09 13.80 13.28 12.91
778 05 32 53.52 06 06 01.1 2 18.20 16.21 14.86 13.15 12.50 12.26
779 05 32 54.29 04 56 05.6 2 20.03 17.40 16.43 14.48 13.85 13.52
780 05 32 54.91 05 32 08.1 3-4 20.13 18.32 17.03 15.15 14.44 14.27
781 05 32 55.17 07 18 03.3 2 18.04 16.16 14.54 12.63 12.00 11.71
782 05 32 55.78 05 37 02.2 2 17.83 16.30 14.54 12.92 12.29 11.98
783 05 32 56.30 06 03 18.9 1 16.75 15.27 14.35 13.04 12.40 12.23
784 05 32 56.43 07 17 44.1 2 19.36 17.20 15.32 13.61 12.98 12.71
785 05 32 56.51 05 34 20.7 2 18.04 16.96 15.39 13.65 13.07 12.78
786 05 32 56.90 05 12 47.7 4 16.44 14.93 14.14 12.57 11.62 11.15
787 05 32 57.01 05 48 56.1 3 19.01 17.39 15.57 13.55 12.90 12.65
788 05 32 57.29 07 18 14.3 2 20.30 17.81 15.19 13.28 12.73 12.44
75-175 05 32 57.92 06 02 42.9 1 17.11 15.54 14.43 12.98 12.32 12.12
789 05 33 00.83 06 27 24.6 2 18.09 16.43 14.94 13.30 12.65 12.42
HS 75-176 98 4-46 39 05 33 01.75 04 49 18.5 4 16.53 15.50 14.34 13.37 12.38 11.52
V466 75-177 100 4-124 40 05 33 02.24 05 26 25.2 2 12.29 11.85 11.20 10.36 9.70 9.23
790 05 33 02.29 05 42 31.0 4 20.76 16.20 14.65 13.93 13.55
791 05 33 02.39 04 55 27.9 3 19.73 17.52 15.89 13.99 13.43 13.12
792 05 33 03.30 06 51 37.8 2 18.26 16.50 14.72 13.07 12.44 12.19
793 05 33 03.35 06 37 32.8 2 17.68 15.88 14.32 12.85 12.27 11.98
75-178 05 33 04.59 04 59 45.7 2 15.83 14.35 13.41 12.31 11.61 11.43
794 05 33 04.87 07 34 14.4 3 19.47 17.74 15.65 13.50 12.85 12.53
795 05 33 05.28 06 25 15.7 1 17.56 15.99 14.27 12.71 12.05 11.82
796 05 33 05.64 07 30 39.1 1 21.20 19.02 15.29 13.73 13.04 12.83
797 05 33 06.39 07 51 45.8 2 18.64 17.33 15.44 13.48 12.84 12.63
798 05 33 06.55 06 43 32.9 2 16.33 13.12 12.42 11.78 11.49
799 05 33 09.86 04 59 48.4 4 20.77 18.83 16.76 14.30 13.83 13.44
V384 76-34 101 4-168 43 05 33 10.53 05 42 24.5 2 15.52 14.38 13.11 11.81 11.03 10.72
800 05 33 11.09 04 28 55.3 1 17.43 15.25 13.74 13.91 13.38 13.11
801 05 33 13.07 07 05 07.1 2 18.82 16.81 15.17 13.36 12.73 12.44
802 05 33 13.45 04 51 32.8 2 16.24 14.88 13.35 12.19 11.52 11.35
803 05 33 14.36 05 13 40.4 1 17.78 15.89 14.10 12.81 12.09 11.90
804 05 33 14.83 06 06 35.8 3 16.95 19.32 17.86 13.33 12.71 12.47
805 05 33 14.92 05 30 33.6 1 17.99 17.43 14.25 12.70 12.08 11.81
806 05 33 14.99 07 16 48.2 1 19.92 17.54 14.72 13.24 12.64 12.32
807 05 33 16.95 05 43 33.1 3 19.94 18.08 16.04 14.00 13.41 13.05
808 05 33 17.96 05 21 38.6 2 18.45 17.24 14.78 13.18 12.56 12.32
76-35 05 33 18.14 04 22 43.3 3 17.14 15.38 14.15 12.93 12.22 11.96
809 05 33 18.39 06 52 16.2 2 18.20 16.59 15.03 13.66 12.98 12.64
810 05 33 19.80 06 04 23.3 3 16.88 15.25 14.09 12.72 12.01 11.83
811 05 33 20.04 05 43 30.7 2 19.14 18.16 15.08 13.68 13.05 12.78
812 05 33 20.22 03 18 10.0 2 18.07 15.37 13.93 13.32 13.04
V542 76-40 4-223 48 05 33 20.99 06 22 33.4 4 16.07 15.19 15.42 12.58 11.65 11.02
813 05 33 21.26 06 01 10.6 3 19.76 17.68 15.66 13.73 13.17 12.89
VW 76-38 4-116 46 05 33 21.37 05 21 34.7 2-3 17.12 14.30 12.67 11.25 10.33 9.77
814 05 33 22.49 05 23 03.1 2 17.26 16.16 14.59 13.07 12.34 12.19
815 05 33 23.03 04 41 01.2 2 17.94 16.03 14.56 13.01 12.34 12.08
816 05 33 23.18 04 20 29.6 1 17.63 16.19 14.40 12.89 12.27 12.02
817 05 33 23.30 05 54 28.2 1 17.49 15.92 14.75 13.23 12.59 12.34
818 05 33 23.45 04 32 50.6 2 17.85 16.30 14.69 12.84 12.21 11.96
819 05 33 23.49 04 42 34.4 3 19.42 17.61 15.49 13.38 12.79 12.45
820 05 33 24.04 04 40 56.1 2 18.42 16.66 15.28 13.39 12.74 12.46
821 05 33 24.81 04 54 11.3 4-5 21.00 17.66 17.86 15.29 14.07 13.16
822 05 33 25.04 04 23 20.2 2 17.07 15.63 14.28 13.03 12.33 12.14
76-41 4-202 49 05 33 25.53 06 06 34.5 4 17.81 16.31 15.46 12.92 11.84 11.03
823 05 33 26.81 05 07 13.3 4 20.06 17.85 18.45 16.08 15.51
824 05 33 28.19 05 04 46.7 1-2 18.09 16.62 14.89 13.19 12.57 12.30
V719 76-42 4-108 51 05 33 28.52 05 17 26.3 2-3 15.13 13.39 11.92 11.14 10.80
825 05 33 30.21 06 04 09.6 2 16.18 14.67 13.87 12.26 11.58 11.36
826 05 33 31.05 04 20 43.6 2 19.53 17.40 15.75 14.14 13.49 13.19
827 05 33 31.20 05 29 57.7 3 19.34 15.26 13.45 12.76 12.44
828 05 33 31.49 06 09 54.2 2-3 18.07 16.41 14.66 12.75 12.03 11.67
829 05 33 31.98 05 14 40.7 2 13.29 17.17 15.32 13.54 12.92 12.68
830 05 33 32.55 06 06 47.7 2 17.33 15.68 14.19 12.45 11.86 11.58
SS 76-48 4-217 61 05 33 33.02 06 18 37.6 4 16.41 14.76 12.69 12.55 11.40 10.73
RZ 76-45 4-97 55 05 33 33.05 05 11 55.5 3-4 16.92 16.54 14.43 12.57 11.77 11.35
831 05 33 33.88 06 33 19.2 2 17.71 16.02 14.73 13.23 12.58 12.27
832 * 05 33 33.90 05 33 26.4 2 17.00 13.82 12.21 11.36 10.96
VX 75-183 103 4-30 53 05 33 34.26 04 43 45.8 3 15.58 13.97 13.36 11.42 10.59 10.12 11
BS 75-184 4-31 54 05 33 34.30 04 44 18.1 1-2 15.33 14.22 12.89 11.43 10.76 10.52
833 05 33 34.40 06 13 52.7 2 16.75 14.99 13.99 12.72 11.98 11.78
834 * 05 33 34.44 05 14 17.7 1 15.97 13.83 12.48 11.73 11.36
VY 76-50 104 4-71 59 05 33 35.89 05 01 32.5 4 16.31 14.35 13.00 11.72 10.89 10.38
835 05 33 36.44 04 49 49.0 2 18.10 16.44 14.95 12.98 12.36 12.12
836 * 05 33 37.05 05 23 07.0 2 18.90 17.25 14.01 12.60 11.83 11.65
837 05 33 37.44 04 10 15.9 2 18.10 16.20 14.79 13.28 12.59 12.30
838 05 33 37.44 06 54 21.2 2 17.21 15.44 14.32 12.71 11.98 11.78
839 05 33 38.16 04 12 31.5 1 12.08 11.40 11.15
840 05 33 38.26 07 18 15.2 2 19.12 16.99 13.91 12.42 11.84 11.56
76-51 4-98 62 05 33 38.56 05 13 12.5 3 19.62 17.11 14.64 12.81 12.04 11.70
841 05 33 38.84 06 32 43.3 2 18.57 16.25 15.19 13.48 12.85 12.64
842 05 33 39.17 04 38 07.3 1 18.50 16.73 15.14 13.39 12.70 12.49
843 05 33 39.77 06 06 03.1 3 19.17 17.26 15.62 13.38 12.77 12.43
844 05 33 40.44 03 03 24.4 3 19.28 17.53 16.20 14.15 13.57 13.26
845 05 33 40.68 05 00 46.4 1 12.52 11.82 11.59
846 05 33 41.59 04 55 59.9 1 18.70 16.69 15.12 13.16 12.51 12.26
847 05 33 41.61 06 06 07.4 4 19.19 17.08 15.81 14.50 13.55 12.80
76-52 4-121 63 05 33 41.68 05 24 04.3 3 18.14 18.16 13.96 12.60 11.81 11.51
4-298 66 05 33 41.94 06 15 48.9 4 18.04 16.59 15.76 14.08 13.32 12.88
848 * 05 33 42.32 05 08 47.3 3 19.57 17.60 15.85 13.97 13.35 13.09
849 05 33 42.95 04 55 43.5 1-2 17.04 15.19 14.03 12.40 11.69 11.47
850 05 33 43.19 04 47 14.3 4 17.04 13.32 12.52 12.13
851 05 33 43.93 06 13 46.3 5 20.33 17.79 18.75 16.66 15.98 14.97
V729 76-53 4-101 67 05 33 44.79 05 14 09.9 2 16.07 14.05 12.01 10.75 10.01 9.65 12
852 * 05 33 44.87 05 11 56.2 2 18.56 16.32 13.83 13.20 12.93
853 05 33 45.00 07 16 27.2 1 21.61 18.81