Spitzer Observations of the Orionis cluster. II. Disks around solar-type and low mass stars
We present IRAC/MIPS Spitzer Space Telescope observations of the solar type and the low mass stellar population of the young ( 5 Myr) Orionis cluster. Combining optical and 2MASS photometry, we identify 436 stars as probable members of the cluster. Given the distance (450 pc) and the age of the cluster, our sample ranges in mass from 2 to objects below the substellar limit. With the addition of the Spitzer mid-infrared data, we have identified 49 stars bearing disks in the stellar cluster. Using spectral energy distribution (SED) slopes, we place objects in several classes: non-excess stars (diskless), stars with optically thick disks, stars with “evolved disks”( with smaller excesses than optically thick disk systems), and “transitional disks” candidates (in which the inner disk is partially or fully cleared). The disk fraction depends on the stellar mass, ranging from 6% for K type stars (-J2) to 27% for stars with spectral type M5 or later (-J4). We confirm the dependence of disk fraction on stellar mass in this age range found in other studies. Regarding clustering levels, the overall fraction of disks in the Orionis cluster is similar to those reported in other stellar groups with ages normally quoted as 5 Myr.
Circumstellar disks, which appear to be a natural byproduct of the process of star formation, play a critical role in the evolution of stars and planetary systems. As these disks evolve, the rate of accretion onto the central star decreases and the gas dissipates, while some of the remaining dust is thought to coalesce into large bodies such as planets and planetesimals. The more crucial processes in the evolution from primordial disks (e.g., optically-thick disks with modest dust coalescence) to planetary systems occur in the age range 1 - 10 Myr, when the dust and gas in the disk is removed (Calvet et al., 2005), second generation dust is created by collisional cascade (Hernandez et al., 2006; Currie et al., 2008), and planets are expected to form (Podosek & Cassen, 1994). Studies with the Spitzer Space Telescope (Werner et al., 2004) of the disk evolution of young, low mass ( 2 ) pre-main sequence stars (T Tauri stars; TTS) in star-forming regions indicate that at 5 Myr about 80% of primordial disks have dissipated (Carpenter et al., 2006; Dahm & Hillenbrand, 2007; Hernandez et al., 2007a, 2008) in agreement with results using near infrared observations (Haisch et al., 2001; Hillenbrand et al., 2006). The disk infrared emission observed in stars bearing primordial disks also declines with age (Hernandez et al., 2007b) suggesting that as time passes, dust grains in the disk collide, stick together, grow to sizes much larger than the wavelength of observation and settle toward the midplane, which reduces the flaring of the disk and thus the amount of energy radiated (Kenyon & Hartmann, 1987; Dullemond & Dominik, 2005; D’Alessio et al., 2006). Finally, 5 Myr is the age at which observations (e.g.; Hernandez et al., 2009) and models (e.g. Kenyon & Bromley, 2004, 2008) suggest that second generation disks, which may trace active planet formation (Greenberg et al., 1978; Backman & Paresce, 1993; Kenyon & Bromley, 2008; Wyatt, 2008; Cieza, 2008), start to dominate the disk population around intermediate mass stars.
The Orionis star forming region is one of the most prominent OB associations in Orion. It includes a ring-like structure of dust and gas of 8-10 degrees in diameter (e.g.; Maddalena & Morris, 1987; Zhang et al., 1989; Dolan & Mathieu, 2002). Several young stellar regions are located near the ring (e.g. B30, B35, LDN1588, LDN1603), in which low mass star formation continues today (Barrado y Navascués et al., 2007a; Mathieu, 2008; Morales-Calderon, 2009). The Orionis cluster (also known as Collinder 69) is located in a region nearly devoid of dense gas near the center of the ring. According to several authors (Maddalena & Morris, 1987; Cunha & Smith, 1996; Dolan & Mathieu, 1999, 2002), Orionis (spectral type O8 III) had a massive companion that became a supernovae (SN), removing nearby molecular gas at the center of the cluster about 1 Myr ago. The ring of dust and gas is then the current location of the swept up material from the SN (e.g.; Mathieu, 2008; Morales-Calderon, 2009).
Because the Orionis cluster is reasonably nearby (450 pc; see Mathieu, 2008) and relatively populous, it represents a valuable laboratory for studies of disk evolution, making statistically significant studies of disk properties in a wide range of stellar masses. Its age of 4-6 Myr (e.g., Murdin & Penston, 1977; Dolan & Mathieu, 2001) represents an intermediate evolutionary stage between two populous stellar clusters located at similar distances in the Orion star formation complex (Bally, 2008) and studied using similar methods to detect and characterize their disks: the Orionis cluster (3 Myr; Hernandez et al., 2007a) and the 25 Orionis aggregate (7-10 Myr; Hernandez et al., 2007b; Briceño et al., 2007).
The Spitzer Space Telescope with its unprecedented sensitivity and spatial resolution in the near- and mid-infrared windows is a powerful tool to expand significantly our understanding of star and planet formation processes; it provides resolved near- and mid-infrared photometry for young stellar populations down to relatively low masses. In an previous paper (Hernandez et al., 2009, hereafter Paper I), we studied the disk population around intermediate mass stars with spectral types F and earlier in the Orionis cluster. In this contribution, we complete a census of the disk population in the cluster studying the infrared excesses produced by disks around stars ranging in mass from solar type stars to the substellar limit. This paper is organized as follows. In Section 2, we describe the observational data in the cluster. In Section 3, we describe the selection of possible members. In Section 4, we present the method for identifying stars with infrared excesses and the classification of the disk population. In Section 5, we present the disk frequencies of the cluster and we compare these frequencies with results from other stellar groups. Finally, we present our conclusions in Section 6.
2.1 Spitzer observations
We are using the Spitzer Space Telescope observations from the Paper I, which include images from the InfraRed Array Camera (IRAC, Fazio et al., 2004) with its four photometric channels (3.6, 4.5, 5.8 & 8.0 µm) and from the 24µm band of the Multiband Imaging Spectrometer for Spitzer (MIPS Rieke et al., 2004).
The region with the complete IRAC data set (hereafter IRAC region) has a size of 57.6′x54.6′ centered at Orionis. More than 40,000 sources were detected in at least one IRAC band using PhotVis (version 1.09), an IDL GUI-based photometry visualization tool developed by R. Gutermuth using the DAOPHOT modules ported to IDL as part of the IDL Astronomy User Library (Landsman, 1993). Final IRAC photometric errors include the uncertainties in the zero-point magnitudes (0.02 mag). MIPS observations cover more than 99% of the IRAC region. The absolute flux calibration uncertainty is 4% (Engelbracht et al., 2007). Our final flux measurements at 24µm are complete down to about 0.8m Jy. The detailed description of the observation, reduction and calibration of the IRAC and MIPS images is given in Paper I.
The Figure 1 illustrates the location of the IRAC region (left-panel), overlaid on a map of dust infrared emission (Schlegel et al., 1998) and CO isocontours (Dame et al., 2001). The space distribution of disk bearing stars of the Orionis cluster (see §4) is shown on a false color image (right panel).
2.2 Optical and Near-IR photometry
We primarily used the V photometry from Dolan & Mathieu (2002, hereafter DM02) to identify possible members in the Orionis cluster. These data were obtained at the Kitt Peak National Observatory using the Mosaic imager on the 0.9m telescope covering an area of 60 centered in the Orionis cluster. Most of the objects in this catalog have magnitudes ranging from V10 to V19. We augmented the optical data set to include the and photometry of 111 very low mass stars and brown dwarfs studied by Barrado y Navascués et al. (2007b, hereafter BN07) not cataloged by DM02. Since there are systematic differences between the and magnitudes of DM02 and BN07 catalogs, we converted the BN07 photometry to the DM02 photometric system. We fitted a straight line in a magnitude-magnitude plot using stars included in both catalogs to obtain the conversion factors needed for each filter.
We combined the optical data set with photometry at J, H and K from the 2MASS Point Source Catalog (Skrutskie et al., 2006). Out of 5168 optical sources in the IRAC region, 4966 stars (96.1%) have 2MASS counterparts and 21 additional sources have near infrared (NIR) photometry from BN07. About 2752 sources in the 2MASS catalog located in the IRAC region do not have optical information. In general, sources in this sample are below the optical detection limit. In appendix A, we present an IRAC/MIPS analysis for this sample to search for sources with infrared excesses.
3 Membership Selection
3.1 Compilation of known members
The Orionis star forming region has been the subject of several studies intended to identify members of its stellar and substellar population and some of these overlap with our IRAC region. Duerr et al. (1982) surveyed a region of 100 around Orionis identifying nearly 100 H emission objects (they used an objective-prism survey). However, most of these objects are located outside the central region, and only two of these objects are in the IRAC region (#1624 and #4407). Dolan & Mathieu (2001, 1999) identified 266 pre-main sequence stars in the Orionis star forming region using the presence of Li i6708 in absorption and radial velocities. They reported a mean radial velocity of 24.5 km s with small dispersion of radial velocities (2.3 km s). Of the 64 sources with Li i in absorption that we have in common with the Dolan & Mathieu (2001, 1999) catalogs (the remaining sources are located outside of IRAC region), 4 stars have radial velocities outside of the 3 range (17.6 - 31.4 km s) that Dolan & Mathieu used for identifying members of the cluster. Since these stars have Li i in absorption (a diagnostic of youth) and binaries can lie off the cluster velocity (e.g., Tobin et al., 2009), we placed them as binaries candidates of the Orionis cluster.
Using optical and near infrared photometry and low resolution spectroscopy, Barrado y Navascués et al. (2004) reported memberships for 170 low mass stars and brown dwarf candidates belonging to the Orionis cluster. This study was improved by BN07 using new deep NIR photometry, IRAC photometry, and additional low resolution spectroscopic data. They reported 19 probable non-members, four stars with dubious membership and 147 bona-fide members of the cluster (hereafter BN07 members), of which more than half have spectroscopic measurements of H and/or spectral types. All of the BN07 members are in the IRAC region. We revisited the disk population of these objects using methods consistent with previous studies of a numbers of star forming regions (Hernandez et al., 2007a, b, 2008), including a better estimation of the effects of errors, for better comparison of disk properties as a function of age and environment (see §4).
Recently, Maxted et al. (2008) and Sacco et al. (2008) studied sub-samples of the BN07 members using high resolution FLAMES (Fiber Large Array Multi Element Spectrograph Pasquini et al., 2002) spectra. Based on radial velocity measurements, Maxted et al. (2008) confirmed 69 BN07 members and rejected 4 using a radial velocity range for members of 22-32 km s. Combining three independent criteria including the radial velocity distribution, the presence of the Li i6708 line and the H line, Sacco et al. (2008) reported membership for 44 BN07 members and 5 stars confirmed as members of the cluster by Dolan & Mathieu (2001). Since Sacco et al. (2008) did not detect Li i in absorption for four BN07 members, they reported them as non-members of the cluster.
Table 1 summarizes the compiled membership information. Column (1) shows the internal running identification number in our sample; columns (2) and (3) provide the stellar coordinates; column (4) shows other names used previously; columns (5) and (6) show spectral types and their references; columns (7) and (8) show radial velocity measurements and their references, columns (9) and (10) indicate whether the star has Li i in absorption and their references, respectively. Column (11) shows membership information compiled from previous studies. Based on column (11), we split the sample of Table 1 in several groups labeled in column 12: (m1) represents confirmed members of the cluster with Li i in absorption and radial velocity in the member range; (m2) represents stars with radial velocity in the member range but no information about Li i (radial velocity members); (m3) represents stars with Li i in absorption and radial velocity out of the member range (binaries candidates); (m4) represents stars with spectral types and photometric data in agreement with the expected trend in color magnitude diagrams (spectral-type members); (m5) represents known members based only on photometric criteria (photometric known candidates); (nm1) represents non members based on photometric criteria, and (nm2) represents non members based on spectroscopic analysis.
3.2 Photometric selection
To select additional candidates to the ones described in §3.1, we used photometric criteria based on their optical-2MASS colors and magnitudes. Figure 2 shows several color magnitude diagrams (CMDs) illustrating our photometric selection. First, we estimated empirical isochrones using the location of confirmed members (open circles) and other members selected using spectroscopic criteria (e.g. open squares; radial velocity members, binaries candidates, and spectral-type members) on these CMDs (hereafter confirmed members, radial velocity members, binaries candidates and spectral-type members are named as “known members” to distinguish from photometric known candidates which are not used in this procedure). Empirical isochrones (dashed lines) were estimated using the median colors (V-J, V-, -J & -) of the known members for 1 magnitude bins in the V-band (upper panels) or in the -band (bottom panels). Standard deviations () were calculated using the differences between the observed colors of the known members and the expected colors from the empirical isochrones. In each CMD, we fitted two lines using a second order polynomial corresponding to the points representing by the median color + 2.5 and by the median color - 2.5, respectively (dotted lines); the regions of probable members are defined between these lines.
Out of 5168 sources with optical photometry within the IRAC region, 4430 sources (86%) are likely background sources since they are located below the regions of probable members in all CMDs. We also found 24 foreground candidates located above the regions of probable members in all CMDs. In the right panels of Figure 2, we plotted stars with no 2MASS counterparts (symbol X). Stars brighter than the magnitude limit in DM02 catalog (V20, R18.7) with no 2MASS counterpart are located below the regions of probable members and thus are likely background stars (220 sources). Stars fainter than the Dolan’s photometric limit were taken from BN07, in which most of them have NIR photometry from deeper images. All of BN07 members are located in the regions of probable members in the lower panels of Figure 2 (there are not V-band magnitudes for the faintest BN07 members).
Our final sample of candidates of the Orionis cluster includes 340 stars located in the regions of probable members in at least three of the four CMDs (297 are located in the four member regions). Additionally, we included 96 stars from BN07 located in the member regions in the lower panels of Figure 2. This sample of 436 stars (hereafter Ori sample) includes 150 known members and 32 photometric known candidates. Since a giant branch crosses the empirical isochrones at V-J2.5, V-1.5, -J1.8 and -0.7, large contamination by no-members of the cluster are expected around these colors.
Table 2 shows IRAC and MIPS photometry for the Ori sample. Column (1) shows the internal running identification number; column (2) provides the 2MASS object name; columns (3) and (4) provide the stellar coordinates; columns (5), (6), (7) and (8) give the IRAC magnitudes in the bands [3.6], [4.5], [5.8] and [8.0], respectively; column (9) gives the flux at 24µm (MIPS band); column (10) shows the disk classification obtained in §4; column (11) shows references for stars studied previously.
Finally, a group of 77 sources are located in the region of probable members in one or two CMDs but appear as likely foreground or background sources in the other CMDs. Infrared properties of these stars with uncertain photometric membership classification are also studied in Appendix A.
4 Disk Population
To characterize the disk population in the Orionis cluster, we need to identify stars in the Ori sample (see §3.2) that exhibit excess emission at the IRAC/MIPS bands. For this purpose, we must properly account for uncertainties and biases in the IRAC/MIPS photometry, particularly near the detection limit of these data (Luhman et al., 2008). In a well-populated sample of stars not strongly affected by extinction, the sum of all these uncertainties and biases (Poisson errors, uncertainties in the zero-point magnitudes, location-dependent variations in the calibration, scatter of photospheric colors among cluster members) is reflected in the spread of colors in a given magnitude among the diskless stars of the cluster, which dominate stellar populations older than 2-3 Myr (e.g., Haisch et al., 2001; Hillenbrand et al., 2006; Hernandez et al., 2007a, 2008). Since a disk produces greater excess emission above the stellar photosphere at longer wavelengths, we selected the bands at 8µm and 24µm to identify and characterize disks in the stellar population of the Orionis cluster. First, we identified disk bearing stars with infrared excesses at 24µm and 8µm in §4.1 and §4.2, respectively. In §4.3 and §4.4, we completed our analysis and classification of the disk population of the Orionis cluster based on the excess emission levels observed in the IRAC/MIPS bands and their SEDs.
4.1 Identifying stars with 24µm excess
Figure 3 illustrates the procedure to identify stars with 24µm infrared excess above the photospheric level (e.g.; Gorlova et al., 2006, 2007; Hernandez et al., 2006, 2007a, 2007b, 2008). The upper panel shows the K- color distribution of stars in the Ori sample detected in the MIPS 24µm image. The distribution of stars with K-1.0 can be described by a Gaussian centered at 0.15 with =0.18. The 3 boundaries (dotted lines in lower panels) represent the photospheric colors; thus stars with excesses at 24µm have colors K-0.69. Since the Orionis cluster has low reddening (0.4; Diplas & Savage, 1994) the R-J color can be used as a proxy of spectral types. We display the location of the spectral type sequence, using the standard R-J colors from Kenyon & Hartmann (1995). The NIR colors from Kenyon & Hartmann (1995) were converted into the 2MASS photometric system using the transformations from Carpenter et al. (2001). We extended the standard R-J colors toward later spectral types using members with spectral types M6 or later reported by BN07. The R-J standard colors were estimated averaging the observed R-J color (BN07) in a given bin of spectral types. There are 4 candidates bearing disks with small excesses at 24µm(K-1.5); three of them have the lower limit of their error bars inside the photospheric region and thus the 24µm excess of these objects is not completely reliable. We have marked these objects in Table 2 as stars with uncertain 24µm excess. Two objects have spectral types M6 or later and are probable brown dwarfs bearing optically thick disks (BN07). There are three stars bearing disks with photometric spectral type earlier than K5. Most stars with 24µm excess (75%) have excess ratio at 24µm (E=; e.g. Paper I, ) larger than 22. The lack of M type stars with photospheric K- colors reflects the limit magnitude of the 24µm MIPS band.
4.2 Identifying stars with 8µm excess
Figure 4 shows the IRAC SED slope versus the [8.0] magnitude for stars in the Ori sample illustrating the procedure to detect infrared excesses at 8µm (e.g.; Lada et al., 2006; Hernandez et al., 2007a, b, 2008). The IRAC SED slope (=) is determined from the [3.6]-[8.0] color. The error bars in are calculated propagating the photometric errors at [3.6] and [8.0]. To determine the photospheric levels, we used the mean error of () for stars within 0.5 magnitude bins in the [8.0] band. The photospheric region (dotted lines) is determined using a 3 criteria from the median values of (long dashed lines). The width of this region depends on the photometric error of the [8.0] magnitude, which dominates the uncertainties in . Thus, a single value of to separate diskless and disk bearing stars based on the IRAC color [3.6]-[8.0] is not useful, especially near the IRAC detection limit (Hernandez et al., 2007a). At the faintest [8.0] magnitudes, the photospheric region is too sparsely populated for a reliable measurement of infrared excesses. For instance, star #7968 ([8.0]14.5) represents the faintest star with a probable disk based on 8µm excess. However, since the detections at 5.8µm and 8.0µm of this star are background-limited and upward fluctuations of the background noise could contaminate these detections, the presence of a disk around this star needs additional confirmation.
For comparison, short-dashed lines in Figure 4 represent the limits used by BN07 to classify disks around stars in the Orionis cluster based on the following criteria (Lada et al., 2006): diskless stars (-2.56), optically thick disks (-1.8), and optically thin disks (-2.56-1.8). The criteria used by BN07 is based on the distribution of the disk population in Taurus (1-2 Myr) from Hartmann et al. (2005), where most of disk bearing stars have -1.8. The right panel of Figure 4 shows the distribution of the disk population in Taurus (1-2 Myr) from Luhman et al. (2010) and supports that disk bearing stars with -1.8 are relatively scarce in Taurus and more frequently observed in older stellar regions (Lada et al., 2006; Hernandez et al., 2007a, b, 2008).
In Figure 4, we also display stars with 24µm excess (open circles) detected in §4.1. In general, stars brighter than [8.0]12.0 with significant excesses at 8µm have excesses at 24µm. There are some disk bearing candidates with error bars inside the photospheric region, the 8µm excess of these objects is uncertain and are identified in Table 2 (see also §4.4). Finally, star #1039 is a relatively bright source ([8.0]9.5) that shows infrared excess only at 8µm ( 5 above the photospheric limit). Visual inspection of the image does not reveal any obvious source of contamination at 8µm. However, at 24µm (where the disk produces greater excess emission) the star #1039 exhibits photospheric fluxes and thus the presence of a disk around this object is highly uncertain.
4.3 Disk diagnostics
Figure 5 displays the distribution of disk bearing stars (with MIPS counterparts) of the Ori sample in a SED slope diagram, generated using the K-[5.8] and [8.0]- colors. The K-[5.8] slope represents disk emission at 5.8µm, while the [8.0]- slope indicates whether the star has a flat (slope0) or rising (slope0) SED at wavelengths greater than 8µm. Using colors from Luhman et al. (2010), we display the SED slope distributions (right-panel and upper panel) and the quartiles (large error bars) of the disk population in Taurus. The dashed line represents a limit where the inner disk emission has not been affected significantly by evolutionary processes (a lower limit of primordial disks for Taurus; Luhman et al., 2010). About 97% of the disk bearing stars in Taurus are located above this line. We use this boundary as a proxy to separate stars bearing optically thick disks (above the dashed line) from other types of disks. We show in Figure 5 the location of five transitional disks in several star forming regions: TW Hya, GM Aur, Coku Tau/4, CS Cha and CVSO 224 (Calvet et al., 2002, 2005; D’Alessio et al., 2005a; Espaillat et al., 2007a, 2008a). Observationally, they are characterized by relatively small excesses at 5.8µm and large excesses at longer wavelengths. Star #4111 can be identified as a transitional disk candidate. Since star #1152 has a rising SED after 8µm and it is near the optically thick disk limit, we also place this star as a transitional disk candidate. The disk of the star Coku Tau/4 is circumbinary, and its structure is a result of tidal truncation due to the binary orbit (Ireland & Kraus, 2008). There is a possibility that our transitional disk candidates can be binary systems and their disks are similar to the disk associated with Coku Tau/4. In addition, Figure 5 shows the location of the newly discovered class of pre-transitional disks (LkCa 15 and UX Tau A), in which gaps in primordial disks rather than holes have been identified (Espaillat et al., 2007b, 2008b; Brown et al., 2008). Two objects (#4021 and #6866) have similar [8.0]- color than the pre-transitional disk LkCa 15, but with less infrared excesses at 5.8µm. We placed these objects as possible pre-transitional disks in the cluster; however, a more detailed study is necessary to reveal the actual nature of their disks.
About 30% of the late type stars bearing disks in the Orionis cluster exhibit relatively small IRAC/MIPS excesses (below the dashed lines and with SED slope [8.0]- 0) indicating that evolutionary processes (e.g. grain growth, dust sedimentation and/or settling) have been at work, generating flatter disk structures (D’Alessio et al., 2006; Dullemond et al., 2007; Manoj, 2010). We identify these sources as evolved disks stars in Table 2. We plotted with squares the three earliest stars with infrared excesses (photometric spectral type earlier than K5). One of these stars (#4155) exhibits modest infrared excess at 5.8µm and 24µm, while the other two stars (#3785 and #7402) exhibit marginal infrared excesses at 24µm and no excesses at 5.8µm. For comparison, we show the locations of the intermediate mass stars bearing disks studied in Paper I; except for the Herbig Ae/Be star HD 245185, these are debris disks candidates, with no excesses in the IRAC bands and varying degrees of excesses at 24µm.
There are 18 disk bearing candidates with excesses at 8µm but without MIPS counterparts (see Figure 4). In general, these stars are below the MIPS detection limit. Only star #3746 could be above the MIPS detection limit; however, it is located near the star Ori which may mask the detection at 24µm. The disks around two stars (#1039 and #7968) are highly uncertain (see §4.2). In summary, based only on the IRAC SED slopes (§4.2), we found 6 stars with optically thick disks, 7 evolved disk stars and 4 stars with uncertain 8µm excess emission. SEDs of individual objects will be detailed in the next section.
4.4 Spectral Energy Distributions
Figures 6 and 8 show SEDs of the candidates bearing disks with and without MIPS counterparts, respectively. Fluxes calculated from optical magnitudes (\al@barrado07b,dolan02; \al@barrado07b,dolan02), 2MASS photometry (J, H K), IRAC bands (3.6, 4.5, 5.8 and 8.0 µm) and the 24µm MIPS band were normalized to the flux in the J band. We sorted the SEDs by photometric spectral types, which where calculated interpolating the R-J color in the standard color sequence (Kenyon & Hartmann, 1995). Since the R-J colors are not corrected by reddening, the photometric spectral type corresponds to a later limit. We display the median SED of the disk population in Taurus. It was constructed from the median colors (2MASS, IRAC and MIPS) of low mass stars (with spectral types K and M) bearing disks from Luhman et al. (2010). We also show the photospheric fluxes for a star with the corresponding photometric spectral type (Kenyon & Hartmann, 1995) normalized to the J band. To compare our results with those from BN07, we display the IRAC/MIPS photometry given by BN07, with their identification number, disk type and spectral type (when is available). In general, disk types identified in §4.3 agree with those given by BN07. Star #1152 (Spectral type M2; thick disk in BN07, ) shows small or no infrared excesses at wavelengths shorter than 8µm and infrared excess at 24µm comparable to stars bearing an optically thick disk; we classified this star as a transitional disk candidate. On the other hand, the star #3597 (Spectral type M4; transition disk in BN07, ) exhibits a decreasing SEDs after 8µm. We classified this object as an evolved disk star.
Three disk bearing stars with photometric spectral types K7 or earlier (#3785 #7402 and #1310) have marginal infrared excesses at 24µm and no excesses detected in the IRAC bands. The disk suggested for these objects needs additional confirmation. If disks are present around these stars, their infrared excesses are comparable to those observed in the early type debris disk candidates (Paper I) indicating probably a similar origin of their infrared emission (e.g Gorlova et al., 2007; Kenyon & Bromley, 2005). The K-type star #4155 clearly exhibits infrared excesses at 8µm and moderate excess at 24µm. The excesses around this star could be explained if the disk is in an intermediate phase evolving from a primordial to a debris disk (evolved disk). The star #5447 was not included in Figure 8, the SED of this thick disk object is similar to that observed in the star #7490 (spectral type M4).
In Figure 8, there are three stars (#7517, #3710 & #2712 with spectral types M0, M6 and M7, respectively) with marginal infrared excesses at 8µm which could be produced by either disk emission or PAH (polycyclic aromatic hydrocarbon) contamination. The IRAC photometry of the star #2712 could be also contaminated by a near bright source (located at 7″) . Based on the IRAC SED slope (Figure 4), the star #7957 is classified as an evolved disk star with a marginal excess at 8µm. However, the SED observed for this source shows excesses in all IRAC bands similar to those observed in sources with thick disks in agreement with the disk type reported by BN07.
There are 16 stars with a thin disk type in BN07 that we classified as diskless star based on the criteria discussed above. Figure 9 shows SEDs for these objects. Several possibilities may support our diskless classification. Three stars only have photometry in the [3.6], [4.5] and [5.8] bands in BN07. Based on the IRAC SED slope, BN07 classified as disk bearing stars objects with -2.56, six of these objects are located in the diskless region in the [3.6]-[4.5] versus [5.8]-[8.0] diagram presented by these authors. As discussed in §4.2, the photospheric region of the IRAC slope depends on the brightness of the star and thus the single value of the IRAC SED slope applied by BN07 to separate diskless and disk bearing stars does not work well, particularly, for the faintest stars. In addition, [8.0] magnitudes given by BN07 are systematically 0.1 magnitudes brighter than our photometry. The K-[8.0] colors of the diskless stars (with photometric spectral types M5 or earlier) in this work are in good agreement with the standard K-[8.0] colors derived from STAR-PET tool available on the Spitzer Science Center website.
5 Disk Frequencies and Disk Diversity of the Orionis CLUSTER
The upper panel in Figure 10 shows disk frequencies as a function of photometric spectral types estimated using the -J color. To reduce the contamination by non-members, frequencies were calculated using the members confirmed by Dolan & Mathieu (2001), BN07, Maxted et al. (2008) and Sacco et al. (2008); see §3.1. We plotted the fractions of confirmed members with optically thick disks (filled circles and solid line) and the fractions of confirmed members bearing any type of disks (open squares and dotted line) including evolved disks and pre-transitional/transitional disks. These fractions decrease for decreasing -J color and flatten up around -J4.5 (spectral types M6-M7). The disk fraction may decline toward later spectral types; however, including the error bars, the data are consistent with no change in disk frequency from M6 to later types
For reference, we plot the masses corresponding to the -J colors along the 5 Myr isochrone of Siess et al. (2000). Since -J color bins represent different ranges in stellar masses, the decrease of disk frequencies toward earlier spectral types indicates that primordial disks dissipate faster as the stellar mass increases. Particularly, for solar type stars the disk frequency is 6%, while for very low mass stars and brown dwarf mass range (0.1) the disk frequency increases to 27%. The decrease of disk frequencies toward higher stellar mass agrees with results in other young stellar populations, e.g.: IC 348 (Lada et al., 2006), Upper Scorpius (Carpenter et al., 2006), the Ori cluster (Hernandez et al., 2007a), and the Ori OB1b subassociation (Hernandez et al., 2007b). For reference, the lower panel of Figure 10 shows the location on the color magnitude diagram of stars bearing disks selected in 3.2. In general, the disk population of stars with spectral type M2 or earlier includes evolved disks objects while optically thick disks are more frequently observed at later spectral types.
Using the lower panel of Figure 10, we can estimate the contamination levels in our sample. We calculated disk fractions in several -J color bins for the confirmed members of the Orionis cluster () and for the entire Ori sample (). Assuming that the source of contamination are photometric candidates without infrared excesses and stars with infrared excesses are members of the cluster bearing disk, we can estimate the contamination level () expected in the Ori sample applying the relation: . Figure 11 shows the contamination level versus the color -J. As discussed in §3.2, the larger contamination level is produced by main sequence stars and by a giant branch that cross the Orionis young stellar population at -J2.5. In general, the level of contamination for M type stars is less than 25%.
Regardless of different environments and clustering levels, the overall disk frequency for M type stars in the Orionis cluster (18.54.0 %) is comparable to those reported in other stellar groups with ages normally quoted as 5 Myr. The more dispersed stellar groups, Upper Scorpius (194 %, Carpenter et al., 2006) and the Orion OB1b subassociation (154 %, Hernandez et al., 2007b), have disk frequencies similar to that observed in the Orionis cluster. This suggests that the clustering levels of stellar groups does not affect significantly the disk frequencies observed at 5 Myr. In particular, the Orion OB1b subassociation and the Orionis cluster have similar stellar mass - disk frequency dependencies (see Paper I, ). The disk frequency for stars later than K5 (stellar mass 1) in the stellar cluster NGC2362 (5 Myr; Dahm & Hillenbrand, 2007) is slightly higher (23.03.4) than that for the Orionis cluster. The number of evolved disks may be overestimated by Dahm & Hillenbrand (2007) as they did not correct for larger photometric errors at faint magnitudes (see 4). Finally, if the supernovae hypothesis proposed by Dolan & Mathieu (1999, 2002) is correct, the similarities in the disk frequencies for several stellar groups suggest that the disk population in the Orionis cluster was not affected significantly by the supernovae.
The detection of evolved disks and pre-transitional/transitional disk candidates in the cluster supports the existence of at least two different pathways in the evolution from primordial disks to second generation disks (e.g., Hernandez et al., 2007a; Cieza, 2008; Manoj, 2010; Currie, 2010). Using the M-type stars with MIPS counterparts (Figures 5 and 6), the frequency of pre-transitional/transitional disks in the Orionis cluster is 13.36.7 (6.74.7 for the transitional disk candidates alone); comparable to that observed in other stellar clusters with ages of 3 Myr or older (see Muzerolle et al., 2010). The relative scarcity of transitional disks can be used to indicate that the phase from primordial disks to second generation disks through “the transitional disk evolutionary pathway” is relatively short. While Sicilia-Aguilar et al. (2008) reported a relatively high fraction (40-50%) of transitional disks for the Coronet cluster (age1Myr), Ercolano et al. (2009) show that this fraction was overestimated, reporting a transitional disk fraction of 1510% for the cluster. On the other hand, one third (33.310.5%) of the disk population in the Orionis cluster is classified as evolved or pre-transitional/transitional disks (hereafter evolved-transitional disks).
Using the same method to classify disk populations, the evolved-transitional disk fractions in the Orionis cluster (3 Myr), the Orion OB1b subassociation (5 Myr) and in the 25 Orionis (8-10 Myr) aggregate are 17.55.3%, 35.314.4% and 40.020.0%, respectively. In contrast, Currie et al. (2009) reported as many as 80% of evolved-transitional disk fraction for the 5 Myr old cluster NGC2362. Based on this, they reported that the timescale for disk dissipation is comparable with the median primordial disk lifetime. However, the reported fractions of evolved disks strongly depend on the limit used to separate primordial and evolved disks. For instance, Currie et al. (2009) used the lower quartile of the median Taurus SED (Furlan et al., 2006) to classify primordial and evolved disks (25% of the disk bearing stars in Taurus are located below this limit). In Figure 5, we used the boundaries defined by Luhman et al. (2010) which follow the upper edges of the color gaps between diskless stars and stars bearing disks in Taurus. Using this criteria, 97% of the disk bearing stars in Taurus are classified as primordial disks (statistically this means a limit of 2). Moreover, the disk population in Taurus shows a large dispersion in disk emission (Hartmann et al., 2005; Luhman et al., 2010; Furlan et al., 2006, 2009). This could be a reflection of the initial properties of these disks, of different rates for disk dispersion processes, and/or of different intrinsic properties of the star-disk systems (e.g., multiplicity, mass of the central object, inclination angle of the disk; Manoj, 2010; Hillenbrand, 2008). Thus, it is difficult to define a reliable criteria to indicate the starting point in the evolution from primordial to second generation disks and, without an individual detailed modeling, the evolved-transitional disk fractions are reference values that can be used to compare different disk populations assuming an certain criteria. In any event, the observation of more evolved-transitional disks stars (given a certain criteria) in older stellar groups does not necessarily imply longer timescales for evolved-transitional disks. An alternative is that star formation has stopped and there is no steady supply of primordial disks (Manoj, 2010). There is also the possibility that the criteria to define primordial disks may be limited and some misclassified evolved disks are still in a primordial disks phase (Luhman et al., 2010; Muzerolle et al., 2010; Manoj, 2010).
6 Summary and Conclusions
We have used the IRAC and MIPS instruments on board the Spitzer Space Telescope to study the disks population of the Orionis cluster. Using optical photometry and members confirmed by spectroscopy, 436 candidates were selected from optical-2MASS color magnitude diagrams. The level of contamination by non-members depends on the spectral type range, showing the lowest level of contamination (25%) for M type stars. Combining optical, 2MASS and Spitzer data and following the procedure used in previous disk census (Hernandez et al., 2007a, b, 2008), we have reported 49 stars bearing disks , 16 of which were detected only in the IRAC bands. Out of 49 disk bearing stars, 38 were reported previously as members of the Orionis cluster (BN07, Dolan & Mathieu, 2001), 11 stars are new members of the cluster based on its infrared excesses and its optical colors and magnitudes.
Based on their SEDs and a SED slope diagram, we classified the disk bearing stars with MIPS counterpart in three classes: 20 thick disk stars, nine evolved disk stars, two transitional disk candidates and two pre-transitional disk candidates. We found that for stars with color R-J3 (later than M3.5) the disk frequencies are 20%-30%, while stars with colors R-J3 (earlier than M3.5) the disk frequencies are 20%. This indicates a mass dependent timescale for disk dissipation in the Orionis cluster, similar to results in other young star populations (Carpenter et al., 2006; Hernandez et al., 2007a, b, 2008; Lada et al., 2006). The overall disk frequency for M type stars in the Orionis cluster (18.54.0) is similar to those reported in stellar groups with similar evolutionary stage: the cluster NGC 2362 (233, Dahm & Hillenbrand, 2007), the OB association Upper Scorpius (194, Carpenter et al., 2006) and the Orion OB1b subassociation (154, Hernandez et al., 2007b). This suggests that the clustering level of the stellar group does not affect significantly the disk frequencies observed at 5 Myr. This work combined with Paper I represents a complete disk census of the stellar population in the Orionis cluster.
Appendix A Additional infrared excess sources
We looked for additional members with infrared excesses of the Orionis cluster analyzing the infrared properties of two samples not included in our photometric selection (§3.2); stars with 2MASS photometry without optical information (§2.2) and stars with uncertain photometric membership derived from the CMDs (§3.2). Out of 2752 2MASS sources in the IRAC region without optical information, 43 sources have detections at 24µm. Out of 77 sources with uncertain photometric membership, 18 sources have detections at 24µm. Following the procedure described in §4.1 and §4.2, Figure 12 shows the diagrams used to identify stars with excesses at 24µm and 8µm for these 61 sources with MIPS counterparts. In the upper panel, we have identified 41 sources with excesses at 24µm. Those sources that do not exhibit excesses at 24µm do not exhibit excesses at 8µm (bottom panel). On the other hand, there are two sources (#1959 and #4244) that do not exhibit excesses at 8µm but exhibit excesses at 24µm. In general, sources with IR excesses are 2MASS objects without optical information, only one (#5968) has uncertain photometric membership. This star is located in the regions of probable members in the V-J versus V and the -J versus diagrams but it appears slightly below from the regions of probable members in the V- versus V and the - versus diagrams.
Visual inspection on the IRAC/MIPS images reveals that most sources with the largest IR excesses are non-stellar. We found that 16 sources are galaxies, and 7 sources have slightly larger PSF (point spread function) widths than other stellar sources on the images (labeled as Stellar?).
Table 3 shows IRAC/MIPS photometry for the 41 sources with infrared excesses. Column (1) shows the internal running identification number; column (2) provides the 2MASS object name; columns (3) and (4) provide the stellar coordinates; columns (5), (6), (7) and (8) give the IRAC magnitudes in the bands [3.6], [4.5], [5.8] and [8.0], respectively; column (9) gives the flux at 24µm (MIPS band); column (10) shows comments based mainly on the visual inspection on the IRAC/MIPS images. Special notes about some interesting objects are given below Table 3.
- Backman & Paresce (1993) Backman, D. E., & Paresce, F. 1993, Protostars and Planets III, 1253
- Bally (2008) Bally, J. 2008, Handbook of Star Forming Regions, Volume I, 459
- Barrado y Navascués et al. (2004) Barrado y Navascués, D., Stauffer, J. R., Bouvier, J., Jayawardhana, R., & Cuillandre, J.-C. 2004, ApJ, 610, 1064
- Barrado y Navascués et al. (2007a) Barrado Y Navascués, D., Stauffer, J. R., Morales-Calderón, M., & Bayo, A. 2007a, Revista Mexicana de Astronomia y Astrofisica Conference Series, 29, 37
- Barrado y Navascués et al. (2007b) Barrado y Navascués, D., et al. 2007b, ApJ, 664, 481 (BN07)
- Bouy et al. (2009) Bouy, H.,/ et al. 2009, A&A, 504, 199
- Briceño et al. (2007) Briceño, C., Hartmann, L., Hernández, J., Calvet, N., Vivas, A. K., Furesz, G., & Szentgyorgyi, A. 2007, ApJ, 661, 1119
- Brown et al. (2008) Brown, J. M., Blake, G. A., Qi, C., Dullemond, C. P., & Wilner, D. J. 2008, ApJ, 675, L109
- Calvet et al. (2002) Calvet, N., D’Alessio, P., Hartmann, L., Wilner, D., Walsh, A., & Sitko, M. 2002, ApJ, 568, 1008
- Calvet et al. (2005) Calvet, N., et al. 2005, ApJ, 630, L185
- Carpenter et al. (2006) Carpenter, J. M., Mamajek, E. E., Hillenbrand, L. A., & Meyer, M. R. 2006, ApJ, 651, L49
- Carpenter et al. (2001) Carpenter, J. M. 2001, AJ, 121, 2851
- Cieza (2008) Cieza, L. A. 2008, Astronomical Society of the Pacific Conference Series, 393, 35
- Cunha & Smith (1996) Cunha, K., & Smith, V. V. 1996, A&A, 309, 892
- Currie et al. (2008) Currie, T., Kenyon, S. J., Balog, Z., Rieke, G., Bragg, A., & Bromley, B. 2008, ApJ, 672, 558
- Currie et al. (2009) Currie, T., Lada, C. J., Plavchan, P., Robitaille, T. P., Irwin, J., & Kenyon, S. J. 2009, ApJ, 698, 1
- Currie (2010) Currie, T. 2010, arXiv:1002.1715
- Dahm & Hillenbrand (2007) Dahm, S. E., & Hillenbrand, L. A. 2007, AJ, 133, 2072
- Dame et al. (2001) Dame, T. M., Hartmann, D., & Thaddeus, P. 2001, ApJ, 547, 792
- Diplas & Savage (1994) Diplas, A., & Savage, B. D. 1994, ApJS, 93, 211
- Dolan & Mathieu (1999) Dolan, C. J., & Mathieu, R. D. 1999, AJ, 118, 2409
- Dolan & Mathieu (2001) Dolan, C. J., & Mathieu, R. D. 2001, AJ, 121, 2124
- Dolan & Mathieu (2002) Dolan, C. J., & Mathieu, R. D. 2002, AJ, 123, 387 (DM02)
- Duerr et al. (1982) Duerr, R., Imhoff, C. L., & Lada, C. J. 1982, ApJ, 261, 135
- D’Alessio et al. (2005a) D’Alessio, P., Hartmann, L., Calvet, N., et al. 2005, ApJ, 621, 461
- D’Alessio et al. (2006) D’Alessio, P., Calvet, N., Hartmann, L., Franco-Hernández, R., & Servín, H. 2006, ApJ, 638, 314
- Dullemond & Dominik (2004) Dullemond, C. P. & Dominik, C. 2004, A&A, 417, 159
- Dullemond & Dominik (2005) Dullemond, C. P., & Dominik, C. 2005, A&A, 434, 971
- Dullemond et al. (2007) Dullemond, C. P., Hollenbach, D., Kamp, I., & D’Alessio, P. 2007, Protostars and Planets V, 555
- Engelbracht et al. (2007) Engelbracht, C. W., et al. 2007, PASP, 119, 994
- Espaillat et al. (2007a) Espaillat, C., et al. 2007a, ApJ, 664, L111
- Espaillat et al. (2007b) Espaillat, C., et al. 2007b, ApJ, 670, L135
- Espaillat et al. (2008a) Espaillat, C., et al. 2008a, ApJ, 689, L145
- Espaillat et al. (2008b) Espaillat, C., Calvet, N., Luhman, K. L., Muzerolle, J., & D’Alessio, P. 2008b, ApJ, 682, L125
- Ercolano et al. (2009) Ercolano, B., Clarke, C. J., & Robitaille, T. P. 2009, MNRAS, 394, L141
- Fazio et al. (2004) Fazio, G. G., et al. 2004, ApJS, 154, 39
- Furlan et al. (2006) Furlan, E., et al. 2006, ApJS, 165, 568
- Furlan et al. (2009) Furlan, E., et al. 2009, ApJ, 703, 1964
- Gordon et al. (2005) Gordon, K. D., et al. 2005, PASP, 117, 503
- Gorlova et al. (2006) Gorlova, N., Rieke, G. H., Muzerolle, J., Stauffer, J. R., Siegler, N., Young, E. T., & Stansberry, J. H. 2006, ApJ, 649, 1028
- Gorlova et al. (2007) Gorlova, N., Balog, Z., Rieke, G. H., Muzerolle, J., Su, K. Y. L., Ivanov, V. D., & Young, E. T. 2007, ApJ, 670, 516
- Greenberg et al. (1978) Greenberg, R., et al. 1978, Icarus, 35, 1
- Gutermuth et al. (2004) Gutermuth, R. A., Megeath, S. T., Muzerolle, J., Allen, L. E., Pipher, J. L., Myers, P. C., & Fazio, G. G. 2004, ApJS, 154, 374
- Haisch et al. (2001) Haisch, K. E., Lada, E. A., & Lada, C. J. 2001, ApJ, 553, L153
- Hartmann et al. (2005) Hartmann, L., Megeath, S. T., Allen, L., Luhman, K., Calvet, N., D’Alessio, P., Franco-Hernandez, R., & Fazio, G. 2005c, ApJ, 629, 881
- Hernandez et al. (2006) Hernández, J., Briceño, C., Calvet, N., Hartmann, L., Muzerolle, J., & Quintero, A. 2006, ApJ, 652, 472
- Hernandez et al. (2007a) Hernández, J., et al. 2007a, ApJ, 662, 1067
- Hernandez et al. (2007b) Hernández, J., et al. 2007b, ApJ, 671, 1784
- Hernandez et al. (2008) Hernández, J., Hartmann, L., Calvet, N., Jeffries, R. D., Gutermuth, R., Muzerolle, J., & Stauffer, J. 2008, ApJ, 686, 1195
- Hernandez et al. (2009) Hernández, J., Calvet, N., Hartmann, L., Muzerolle, J., Gutermuth, R., & Stauffer, J. 2009, ApJ, 707, 705 (Paper I (Paper I)
- Hillenbrand et al. (2006) Hillenbrand, L. A., 2006, A Decade of Discovery: Planets Around Other Stars (eds. M. Livio), STScI Symposium Series #19
- Hillenbrand (2008) Hillenbrand, L. A. 2008, Physica Scripta Volume T, 130, 014024
- Ireland & Kraus (2008) Ireland, M. J., & Kraus, A. L. 2008, ApJ, 678, L59
- Kenyon & Hartmann (1995) Kenyon, S. J. & Hartmann, L. 1995, ApJS, 101, 117
- Kenyon & Hartmann (1987) Kenyon, S. J., & Hartmann, L. 1987, ApJ, 323, 714
- Kenyon & Bromley (2005) Kenyon, S. J., & Bromley, B. C. 2005, AJ, 130, 269
- Kenyon & Bromley (2004) Kenyon, S. J., & Bromley, B. C. 2004, AJ, 127, 513
- Kenyon & Bromley (2008) Kenyon, S. J., & Bromley, B. C. 2008, ApJS, 179, 451
- Kharchenko & Roeser (2009) Kharchenko, N. V., & Roeser, S. 2009, VizieR Online Data Catalog, 1280, 0
- Lada et al. (2006) Lada, C. J., et al. 2006, AJ, 131, 1574
- Landsman (1993) Landsman, W. B. 1993, ASP Conf. Ser. 52: Astronomical Data Analysis Software and Systems II, 52, 246
- Lindroos (1985) Lindroos, K. P. 1985, A&AS, 60, 183
- Luhman et al. (2008) Luhman, K. L., Hernández, J., Downes, J. J., Hartmann, L., & Briceño, C. 2008, ApJ, 688, 362
- Luhman et al. (2010) Luhman, K. L., Allen, P. R., Espaillat, C., Hartmann, L., & Calvet, N. 2010, ApJS, 186, 111
- Maddalena & Morris (1987) Maddalena, R. J., & Morris, M. 1987, ApJ, 323, 179
- Manoj (2010) Manoj, P. 2010, arXiv:1003.5933
- Mathieu (2008) Mathieu, R. D. 2008, Handbook of Star Forming Regions, Volume I, 757
- Maxted et al. (2008) Maxted, P. F. L., Jeffries, R. D., Oliveira, J. M., Naylor, T., & Jackson, R. J. 2008, MNRAS, 385, 2210
- Morales-Calderon (2009) Morales-Calderon, M. 2009, PhD thesis, Universidad autÃ³noma de Madrid, Spain
- Murdin & Penston (1977) Murdin, P., & Penston, M. V. 1977, MNRAS, 181, 657
- Muzerolle et al. (2010) Muzerolle, J., Allen, L. E., Megeath, S. T., Hernández, J., & Gutermuth, R. A. 2010, ApJ, 708, 1107
- Pasquini et al. (2002) Pasquini, L., et al. 2002, The Messenger, 110, 1
- Podosek & Cassen (1994) Podosek, F. A., & Cassen, P. 1994, Meteoritics, 29, 6
- Reach et al. (2006) Reach, W. et al. 2006, Infrared Array Camera Data Handbook, version 3.0, Spitzer Science Center, California Institute of Technology, Pasadena, California 91125 USA.
- Rieke et al. (2004) Rieke, G. H., et al, 2004, ApJS, 154, 25
- Sacco et al. (2008) Sacco, G. G., Franciosini, E., Randich, S., & Pallavicini, R. 2008, A&A, 488, 167
- Schlegel et al. (1998) Schlegel, D. J., Finkbeiner, D. P., & Davis, M. 1998, ApJ, 500, 525
- Sicilia-Aguilar et al. (2008) Sicilia-Aguilar, A., Henning, T., Juhász, A., Bouwman, J., Garmire, G., & Garmire, A. 2008, ApJ, 687, 1145
- Siess et al. (2000) Siess, L., Dufour, E., & Forestini, M. 2000, A&A, 358, 593
- Skrutskie et al. (2006) Skrutskie, M. F., et al. 2006, AJ, 131, 1163
- Tobin et al. (2009) Tobin, J. J., Hartmann, L., Furesz, G., Mateo, M., & Megeath, S. T. 2009, ApJ, 697, 1103
- Weidenschilling (1997) Weidenschilling, S. J. 1997, Icarus, 127, 290
- Werner et al. (2004) Werner, M. W., et al. 2004, ApJS, 154, 1
- Wyatt (2008) Wyatt, M. C. 2008, ARA&A, 46, 339
- Zhang et al. (1989) Zhang, C. Y., Laureijs, R. J., Chlewicki, G., Wesselius, P. R., & Clark, F. O. 1989, A&A, 218, 231
Note. – Table 1 is published in its entirety in the electronic edition of the Astrophysical Journal. A portion is shown here for guidance regarding its form and content. footnotetext: References: (1) Dolan & Mathieu (2001); (2) Barrado y Navascués et al. (2007b); (3) Maxted et al. (2008); (4) Sacco et al. (2008) 11footnotetext: Column 11: (1a) and (1b) represent stars with in absorption from Dolan & Mathieu (2001) and Radial Velocity in the members range and out the member range,respectively; (2a), (2b), (2c) and (2d) represent the member flags Y, Y?, N?, and N, respectively, from Barrado y Navascués et al. (2007b); (3a) members, (3b) no members from the radial velocity analysis of Maxted et al. (2008); (4a) and (4b) member and no members from the and radial velocity analysis of Sacco et al. (2008) 22footnotetext: Column 12: (m1) radial velocity members with in absorption; (m2) Radial velocity members with no information; (m3) stars with in absorption and radial velocity out of member range; (m4) Both spectral type and photometric data in aggrement with cluster sequence; (m5) photometric members; (nm1) non-members based on photometric analysis; (nm2) non-members based in spectroscopic analysis
|deg||deg||mag||mag||mag||mag||mJy||reference88See Table 1|
|30||05331224+0934464||83.30102||9.57958||10.71 0.02||10.71 0.02||10.68 0.02||10.65 0.02||-99.99 99.990||diskless|
|42||05331308+0937597||83.30452||9.63328||11.50 0.02||11.52 0.02||11.43 0.03||11.45 0.03||-99.99 99.990||diskless|
|65||05331515+0950301||83.31313||9.84172||11.45 0.02||11.24 0.02||11.08 0.03||10.64 0.02||3.96 0.890||Ev/Thk|
|208||05332084+0958048||83.33684||9.96803||11.69 0.02||11.73 0.02||11.63 0.03||11.63 0.03||-99.99 99.990||diskless|
|296||05332402+1019535||83.35012||10.33153||10.78 0.02||10.75 0.02||10.81 0.02||10.77 0.02||-99.99 99.990||diskless|
|328||05332480+1012116||83.35334||10.20324||10.30 0.02||10.26 0.02||10.22 0.02||10.20 0.02||-99.99 99.990||diskless|
|623||05333353+0935494||83.38974||9.59708||10.44 0.02||10.43 0.02||10.46 0.02||10.42 0.02||-99.99 99.990||diskless|
|630||05333378+1009233||83.39077||10.15650||10.73 0.02||10.78 0.02||10.76 0.02||10.62 0.02||-99.99 99.990||diskless|
|7662||05370084+0949045||84.25352||9.81792||9.94 0.02||9.93 0.02||9.87 0.02||9.88 0.02||-99.99 99.990||diskless|
|7689||05370204+1014447||84.25851||10.24577||11.07 0.02||11.12 0.02||11.10 0.03||11.11 0.03||-99.99 99.990||diskless|
|7701||05370265+1003583||84.26104||10.06620||11.49 0.02||11.52 0.02||11.47 0.03||11.52 0.03||-99.99 99.990||diskless|
|7957||83.65117||9.92561||15.04 0.03||14.76 0.04||14.19 0.13||14.20 0.14||-99.99 99.990||Thk3,63,6footnotemark:||2a|
|7968||83.80912||9.90209||16.08 0.07||15.86 0.08||16.23 0.73||14.64 0.28||-99.99 99.990||diskless44Faint stars with not reliable excesses at 5.8µm & 8.0µm||2a|
Note. – Table 2 is published in its entirety in the electronic edition of the Astrophysical Journal. A portion is shown here for guidance regarding its form and content. Note. – Column 10: Thk-star with an optically thick disk; TD-transitional disk candidate; PTD-pre transitional disk candidate; EV-star with an evolved (flat) disk; diskless-star with no infrared excesses. 11footnotetext: stars with uncertain 24µm excess 22footnotetext: stars with uncertain 8µm excess 33footnotetext: stars without 24µm counterpart 55footnotetext: Star with moderate IR excess at 8.0µm but the 24µm flux is consistent with the photospheric fluxes 66footnotetext: Classified as evolved disk star from the IRAC SED slope 77footnotetext: The star Orionis may mask the detection at 24µm
|241||05332198+1002019||83.34160||10.03387||12.928 0.022||12.700 0.023||12.464 0.038||11.949 0.038||1.42 0.85|
|336||05332499+0937360||83.35415||9.62667||13.658 0.025||13.439 0.028||13.467 0.082||11.177 0.027||1.89 0.98||Galaxy|
|387||05332696+1001394||83.36234||10.02764||14.417 0.031||13.833 0.031||13.306 0.068||12.393 0.054||1.87 0.93|
|415||05332785+0933527||83.36605||9.56464||14.469 0.030||14.366 0.037||13.560 0.070||11.211 0.027||2.00 0.86||Galaxy|
|547||05333119+0958575||83.38000||9.98265||14.919 0.034||14.793 0.042||14.491 0.168||12.210 0.049||1.79 0.95||Stellar?|
|685||05333531+1008261||83.39715||10.14059||14.425 0.029||14.208 0.034||13.938 0.084||13.314 0.073||1.11 0.82|
|907||05334256+1003478||83.42737||10.06328||13.812 0.025||13.169 0.025||12.567 0.040||11.172 0.026||5.16 0.85|
|1110||05334885+0959544||83.45355||9.99847||14.251 0.029||14.076 0.033||13.710 0.079||11.094 0.030||2.12 0.98||Galaxy|
|1959||05341507+1019091||83.56283||10.31921||7.599 0.020||7.492 0.020||7.458 0.020||7.472 0.020||9.07 1.60|
|2040||05341771+0939224||83.57379||9.65623||12.591 0.022||12.295 0.022||11.936 0.031||11.319 0.028||1.59 0.88|
|2191||05342233+1023279||83.59305||10.39108||15.027 0.036||14.506 0.036||14.215 0.114||11.410 0.032||3.08 0.89||Stellar?|
|2773||05344013+0956435||83.66724||9.94544||13.494 0.024||13.355 0.027||12.472 0.047||9.659 0.022||11.80 1.39||Galaxy|
|3212||05345260+0955500||83.71918||9.93058||11.323 0.021||10.967 0.021||10.677 0.023||10.179 0.022||9.22 1.02|
|3245||05345340+0948500||83.72252||9.81390||13.963 0.026||13.794 0.029||13.382 0.071||10.742 0.025||4.16 1.07||Galaxy|
|3268||05345389+0946268||83.72455||9.77411||14.546 0.030||14.046 0.032||13.646 0.080||11.561 0.032||5.27 0.82||Stellar?|
|3323||05345526+0935368||83.73026||9.59357||14.425 0.030||14.036 0.031||13.861 0.098||11.505 0.033||2.24 0.97||Galaxy|
|3451||05345860+0937287||83.74419||9.62465||14.668 0.030||14.222 0.032||13.861 0.090||11.837 0.037||2.06 0.87||Galaxy|
|3778||05350816+0955344||83.78401||9.92623||8.945 0.020||8.799 0.021||8.390 0.024||6.738 0.023||3149.89 313.33|
|3786||05350835+0935535||83.78479||9.59822||12.968 0.022||12.754 0.023||12.597 0.042||11.896 0.035||1.96 0.84|
|3822||05350931+0959112||83.78880||9.98646||13.424 0.024||13.351 0.028||12.466 0.041||9.727 0.022||8.22 1.42||Galaxy|
|3910||05351190+0951178||83.79960||9.85495||13.795 0.028||13.756 0.033||13.541 0.081||11.164 0.034||1.88 0.64||Galaxy|
|3933||05351228+0955131||83.80120||9.92033||12.079 0.022||11.719 0.022||11.429 0.028||10.992 0.026||3.17 1.45|
|4013||05351511+0943596||83.81300||9.73324||14.648 0.032||14.249 0.036||13.982 0.101||11.653 0.034||2.43 0.88||Stellar?|
|4057||05351649+0954372||83.81873||9.91034||13.555 0.025||13.356 0.027||12.502 0.039||9.883 0.022||5.43 1.04||Galaxy|
|4244||05352114+1005584||83.83810||10.09958||14.206 0.027||14.169 0.033||14.065 0.099||14.055 0.179||1.48 0.81|
|4321||05352343+0955335||83.84766||9.92599||14.512 0.029||14.199 0.033||13.823 0.097||11.172 0.028||2.49 0.50||Galaxy|
|4405||05352535+0954476||83.85565||9.91324||12.630 0.022||12.329 0.022||12.008 0.032||11.165 0.026||12.28 0.59|
|4527||05352872+0934328||83.86968||9.57579||13.292 0.023||13.098 0.025||12.877 0.048||12.164 0.042||1.32 0.85|
|4693||05353347+1002087||83.88948||10.03576||14.380 0.032||13.985 0.033||14.192 0.118||12.327 0.047||0.94 0.54||Galaxy|
|5045||05354444+0945520||83.93517||9.76446||12.392 0.021||12.133 0.022||11.913 0.030||11.209 0.026||4.40 0.88|
|5367||05355400+1003458||83.97500||10.06274||14.576 0.032||14.069 0.033||14.078 0.121||11.263 0.026||3.37 0.92||Galaxy|
|5541||05355903+1013175||83.99598||10.22153||13.765 0.024||13.527 0.026||13.332 0.064||12.759 0.068||1.06 0.84|
|5582||05360034+0956488||84.00143||9.94691||14.045 0.026||13.960 0.030||13.387 0.069||10.849 0.024||2.48 0.87||Galaxy|
|5968||05361125+0946263||84.04689||9.77397||11.437 0.021||11.045 0.021||10.733 0.023||10.422 0.023||3.35 0.85|
|6047||05361360+0930386||84.05668||9.51073||14.862 0.033||14.408 0.034||14.287 0.116||12.883 0.054||1.53 0.83||Stellar?|
|6638||05363109+0953262||84.12955||9.89062||13.904 0.027||13.739 0.030||13.495 0.068||10.884 0.024||2.95 0.87||Stellar?|
|6797||05363604+0934545||84.15020||9.58182||13.527 0.024||13.337 0.026||13.110 0.053||12.438 0.048||1.01 0.83|
|7039||05364332+0957016||84.18051||9.95045||13.992 0.026||13.785 0.030||13.343 0.058||10.489 0.023||6.50 1.01||Galaxy|
|7179||05364695+0933541||84.19565||9.56505||15.090 0.034||14.993 0.048||14.735 0.195||11.747 0.031||1.25 0.83||Stellar?|
|7251||05364890+0955423||84.20378||9.92844||12.817 0.022||12.534 0.023||12.179 0.034||11.387 0.028||2.61 0.88|
|7615||05365897+0956307||84.24572||9.94187||14.314 0.029||14.053 0.034||13.940 0.099||11.866 0.038||1.62 0.49||Galaxy|
Note. – footnotetext: Star #3778 (HD36861 C): is located about 30″south of the star Orionis. This F8 V star is member of the central multiple system of the cluster (Lindroos, 1985; Bouy et al., 2009). Its strong infrared excess at 8 µm and 24 µm suggest that #3778 is an intermediate mass star surrounded by an optically thick disk. footnotetext: Star #1959 (NLTT15297): is a double system reported as a high proper motion star. Its optical colors reported in SIMBAD suggest that #1959 is a foreground system. This star does not have photometry in the optical database used in §3.2. footnotetext: Star #5968: is the only possible disk bearing star with discrepant photometric membership in §3.2 (see text) footnotetext: Star #4244: is the faintest object with excess at 24 µm. Since this object does not exhibit excess at 8µm, #4244 could be a transitional disk around a very low mass object in the Orionis cluster. Additional observations are required to confirm membership for this object.