Table 6.
Overview of the recent literature to which we compare the SigMA Sco-Cen clustering results in more detail.
| Reference | Sect. | Data | Studied area | Number statistics |
|||||
|---|---|---|---|---|---|---|---|---|---|
| Nr. in Ref. (a) | SigMA(b) | Matches (c) | Recovered (d) | Rejected (d) | New (d) | ||||
| Damiani et al. (2019)(e) | 5.2.1 | DR2 | (l = 360° to 280°, b = 0° to 30° ) OR | 10 421 | 11 796 | 9328 | 89.5% | 10.5% | 20.9% |
| (l = 315° to 280°, b = −10° to 0° ) | 1732 clustered (17%) | 1719 | 99.2% | 0.8% | |||||
| FOV = 2750 deg2, d < 200 pc | 8689 diffuse (83%) | 7609 | 87.6% | 12.4% | |||||
| Kerr et al. (2021)(f) | 5.2.2 | DR2 | The whole TLC22 stellar group | 7394 | 12 669 | 6270 | 84.8% | 15.2% | 50.5% |
| TLC22 without EOM 1–5 | 7138 | 12 669 | 6270 | 87.8% | 12.2% | ||||
| 22 EOMs of TLC22 (without EOM 1–5) | 3453 | 12 669 | 3447 | 99.8% | 0.2% | ||||
| Schmitt et al. (2022)(g) | 5.2.3 | EDR3 and | de Zeeuw et al. (1999) borders: | 6150 | 11 348 | 3385 | 55.0% | 45.0% | 70.2% |
| eROSITA | US (l = 343° to 360°, b = 10° to 30° ) OR | ∼69% vel-clustered | 3385 | ∼80% | ∼20% | ||||
| UCL (l = 312° to 350°, b = 0° to 25° ) OR | ∼26% vel-diffuse | 0 | |||||||
| LCC (l = 285° to 312°, b = −10° to 22° ), | ∼5% IC 2602 | 0 | |||||||
| FOV = 2050 deg2, d ∼ 60–200 pc | |||||||||
| Luhman (2022) | 5.2.4 | EDR3 | l = 2° to 285°, b = −12° to 35°, | 10 509 | 12 215 | 9838 | 93.6% | 6.4% | 19.5% |
| FOV = 3252 deg2, d ∼ 90–250 pc | |||||||||
| Žerjal et al. (2023) | 5.2.5 | DR2 | l = 40° to 240°, b = −60° to 70°, | 8185 | 12 943 | 7671 | 93.7% | 6.3% | 40.7% |
| FOV = 36 400 deg2, d ∼ 83–200 pc | |||||||||
| Squicciarini et al. (2021)(h) | 5.2.6 | EDR3 | α = 236° to 251°, δ = −29° to −16° | 2745 | 2717 | 2575 | 93.8% | 6.2% | 5.2% |
| (only US, | FOV = 195 deg2, d ∼ 125–175 pc | 1442 clustered (53%) | 1435 | 99.5% | 0.5% | ||||
| subsample with RVs) | 1303 diffuse (47%) | 1140 | 87.5% | 12.5% | |||||
| Miret-Roig et al. (2022a)(i) | 5.2.7 | DR3 | α = 235° to 252°, δ = −30° to −17° | 2810 | 3089 | 2683 | 95.5% | 4.5% | 13.1% |
| (only US, | FOV = 221 deg2, d ∼ 80–200 pc | 2190 5D (78%) | 2145 | 97.9% | 2.1% | ||||
| subsample with RVs) | 670 6D (24%) | 667 | 99.6% | 0.4% | |||||
| 620 Rest (22%) | 538 | 86.8% | 13.2% | ||||||
| Briceño-Morales & Chanamé (2023)(j) | 5.2.8 | EDR3 | l = 343° to 360°, b = 10° to 30° | 3004 | 3439 | 2720 | 90.5% | 9.5% | 20.9% |
| (only US, | FOV = 340 deg2, d < 200 pc | 995 clustered (33.1%) | 989 | 99.4% | 0.6% | ||||
| subsample with RVs) | 2009 diffuse (66.9%) | 1731 | 86.2% | 13.8% | |||||
Notes.
Number of stellar members from the given reference. If there was a distinction in the literature between members in a more clustered or diffuse mode (which are generally differently defined in each reference), then the numbers are given below.
Number of stellar cluster members from SigMA in the given studied area (volume), out of the total 13 103 SigMA stellar cluster members.
Number of matches between the given reference and the SigMA clusters. If a distinct comparison with clustered or diffuse sources was given in the literature, then the numbers and matches with these are given below.
The fraction of recovered, rejected (or missed), and new sources are calculated by comparing the number of matched sources (Col. c) to the sample sizes from the literature (Col. a) or the SigMA sources in the same FOV (Col. b).
For DPP19 we only give the number of sources within their clustered or diffuse populations within 1000/ϖEDR3 < 200 pc after a cross-match with Gaia EDR3, and without IC 2602.
For KRK21, we do not give the surveyed area since they extracted the clusters from all-sky data within 333 pc from the Sun. Still, we show a comparison to their whole TLC22 group (their main Sco-Cen group). We compare to 12 669 sources without Cham, Oph-SE, and Oph-NE since these are not contained within the TLC22 volume. Below we compare to TLC22, excluding their older EOM groups, and finally to the TLC22 members that are contained in one of the younger EOM groups (again without older EOM groups).
The X-ray-selected sources from SCF22 include velocity-clustered and velocity-diffuse sources. The separation of these was applied by us by hand, guided by Fig. 7 in SCF22. Hence, the fractions are only given roughly. The fraction of potential IC 2602 members is also given. The SigMA clusters have only matches with their velocity-clustered population.
SGB21 only studied the US region, finding sources in a more clustered mode and sources in a more diffuse mode, while the latter is simply the residuals of their clustering procedure. They study a subsample of sources with vr information in the 6D phase space (∼28%), which is not further discussed in this work.
MR22 only studied the US region. They study a subsample of sources with vr information in the 6D phase space (∼30%). The numbers of sources in the MR22 bona fide 5D and bona fide 6D samples are listed separately, with “Rest” being sources in neither of the two. Note that the 6D sample is contained within the 5D sample.
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