Abstract
Pisces–Eridanus (Psc–Eri), a nearby (d ≃ 80–226 pc) stellar stream stretching across ≈120° of the sky, was recently discovered with Gaia data. The stream was claimed to be ≈1 Gyr old, which would make it an exceptional discovery for stellar astrophysics, as star clusters of that age are rare and tend to be distant, limiting their utility as benchmark samples. We test this old age for Psc–Eri in two ways. First, we compare the rotation periods for 101 low-mass members (measured using time-series photometry from the Transiting Exoplanet Survey Satellite) to those of well-studied open clusters. Second, we identify 34 new high-mass candidate members, including the notable stars λ Tauri (an Algol-type eclipsing binary) and HD 1160 (host to a directly imaged object near the hydrogen-burning limit). We conduct an isochronal analysis of the color–magnitude data for these highest-mass members, again comparing our results to those for open clusters. Both analyses show that the stream has an age consistent with that of the Pleiades, i.e., ≈120 Myr. This makes the Psc–Eri stream an exciting source of young benchmarkable stars and, potentially, exoplanets located in a more diffuse environment that is distinct from that of the Pleiades and of other dense star clusters.
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1. Introduction
Star clusters at least 1 Gyr in age are rare, and tend to be located at large distances from Earth (e.g., Dias et al. 2002; Kharchenko et al. 2005). This is a shame, because such clusters serve as critical benchmarks for stellar astrophysics. Recently, Meingast et al. (2019) announced the discovery of a stellar stream that stretches 120° across the sky, and spans ≈400 pc in space. This discovery was made possible by the precise astrometry, radial velocities (RVs), and photometry included in the Gaia mission's second data release (DR2; Gaia Collaboration et al. 2018a). Discovery of the Pisces–Eridanus stream (Psc–Eri)7 was somewhat of a surprise given its combination of old age (≈1 Gyr) and proximity (d = 129 ± 32 pc from Earth; median and standard deviation of the 256 published members; the full range is d ≃ 80–226 pc). For context, we list the distance moduli for notable benchmark open clusters along with their ages in Table 1. Figure 1 plots the age and distance to a selection of clusters with measured rotation periods (Prot), which further highlights how remarkable and useful a 1 Gyr cluster this close to Earth would be.
Table 1. Ages and Distance Moduli for Notable Benchmark Star Clusters with Rotation Data
Name | m − M | Age (Gyr) | Age Reference |
---|---|---|---|
Pleiades | 5.67 | 0.120 | Stauffer et al. (1998) a |
Praesepe | 6.35 | 0.670 | Douglas et al. (2019) |
Hyades | 3.37 | 0.730 | Douglas et al. (2019) |
NGC 6811 | 10.20 | 1.0 | Curtis et al. (2019) |
NGC 752 | 8.20 | 1.4 | Agüeros et al. (2018) |
Ruprecht 147 | 7.40 | 2.7 | Torres et al. (2018) |
M67 | 9.72 | 4.0 | Önehag et al. (2011) |
Notes. These distance moduli only account for distance, and do not include visual extinction.
aThe Pleiades age has been constrained with the lithium depletion boundary to 125–130 Myr by Stauffer et al. (1998) and 115 ± 5 Myr by Dahm (2015). Recent isochrone analyses by Gossage et al. (2018) found 110–160 Myr; Cummings & Kalirai (2018) found 115–135 Myr. We adopt 120 Myr for this work.Download table as: ASCIITypeset image
If Psc–Eri's age is truly 1 Gyr, it would be the oldest coeval stellar population within 300 pc. This would open up many avenues for research that are difficult or impossible to pursue with the 1-Gyr-old benchmark cluster NGC 6811 (Sandquist et al. 2016; Curtis et al. 2019), currently the only open cluster of this age we have been able to study in detail. For example, Meibom et al. (2013) discovered two sub-Neptune exoplanets in NGC 6811, but these are too faint for efficient RV follow-up. It is also challenging to measure chromospheric Ca ii H & K activity indices for FGK stars in NGC 6811: those stars are faint (a solar twin is V ≈ 15), and the interstellar Ca ii H & K contamination is difficult to mitigate (Curtis 2017). Finally, Psc–Eri could be an interesting test case for demonstrating the chemical tagging technique needed for Galactic archeology (Freeman & Bland-Hawthorn 2002).
Given the potential value of this population of stars, it is important to examine its age to see if it can serve as a benchmark for old stars. A similar exercise with the purportedly old nearby cluster Ruprecht 147 proved very fruitful (Curtis et al. 2013; Curtis 2016), while the exploration of another candidate old cluster, Lodén 1, showed that it did not exist (Han et al. 2016).
We use gyrochronology, the age-dating method based on stellar rotation and magnetic braking (Barnes 2003; Soderblom 2010), to test the existence and coevality of the Psc–Eri stream. Coeval stars form well-defined sequences in their color–period diagrams, analogous to the main sequence in a color–magnitude diagram (CMD). But color–period sequences are much more sensitive to age, as the full sequence evolves measurably in time as stars spin down, while only the massive end of the main sequence shows significant evolution in temperature and luminosity. If the stars are coeval, a gyrochronology analysis will also yield a precise age for the Psc–Eri stream. We conduct this experiment in Section 2, where we extract and analyze light curves for 101 members of the stream observed by the Transiting Exoplanet Survey Satellite (TESS). We find that the resulting Prot distribution precisely overlaps the Pleiades distribution, making it ≈120 Myr old.
In Section 3, we reinterpret the CMD of the stream by noting that Gaia DR2 measured RVs for stars with Teff ≲ 7000 K, which biased the Meingast et al. (2019) membership census. The CMD of the Psc–Eri stream closely matches that of the Pleiades, except that its membership is truncated due to this RV bias. Combining Gaia DR2 data with literature RVs, we identify 22 new candidates that are warmer than the stars in the Meingast et al. (2019) sample, and another 12 that lack RVs but are comoving in proper motion within 10 pc of known members. These stars closely follow the upper main sequence of the Pleiades, providing further evidence of the Psc–Eri stream's young age. We also briefly discuss the stream's formation in Section 3, before concluding in Section 4.
2. Age-dating the Psc–Eri Stream with Gyrochronology
2.1. Rotation Period Measurements with TESS
TESS (Ricker et al. 2015) is currently conducting a year-long photometric monitoring campaign of the southern sky. TESS scans the sky in a series of sectors for ≈27 days at a time. Full-frame images (FFI) are recorded with a 30 m cadence. As of writing, FFI data for the first five sectors have been released to the Mikulski Archive for Space Telescopes (MAST).
Meingast et al. (2019) published a list of 256 candidate members of the Psc–Eri stream. We used the Web TESS Viewing Tool (WTV)8 to identify stars observed during Sectors 1–5, and we found 154 with data from at least one sector. We downloaded 20 × 20 pixel cutouts of the FFI images centered on each target using the TESScut tool hosted at MAST (Brasseur et al. 2019).9 Next, we used the IDL procedure aper.pro from the IDL Astronomy User's Library (Landsman 1993) to perform aperture photometry on all epochs in the image stack produced by TESScut. We used a circular aperture with a three-pixel radius (≈1' based on TESS's ≈21'' pixel scale).
The resulting light curves overwhelmingly showed clear spot modulation with relatively large amplitudes and short periods compared to our expectations from the 1 Gyr NGC 6811 data from Kepler (Meibom et al. 2011a; Curtis et al. 2019). We were able to measure Prot without performing any additional calibration on these light curves. Figures 2 and 3 show examples of TESS light curves for stream members produced following this simple procedure.
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Standard image High-resolution image2.2. The Color–Period Diagram
We measured rotation periods for 101 stars using Lomb–Scargle periodograms (Scargle 1982; Press & Rybicki 1989). After extracting each light curve and computing the periodogram, we visually inspected the results (see Figures 2 and 3) to ensure the accuracy of our measurements. On only three occasions did we double the Lomb–Scargle period to correct for a one-half-period harmonic error, which we visually identified by noticing asymmetry in the depths of alternating minima and other subtle morphological asymmetries. The measurements are provided in Table 2.
Eleven stars were observed twice, in neighboring sectors, and for these we find consistent periods across sectors. Figure 3 shows an example where we stitched the light curves from two sectors together, and found a more precise period than attained from either sector separately (based on the width of the periodogram peak). Stitching the light curves together was simplified by the fact that multiple maxima and minima were captured in each sector, which meant that no reference stars were needed to normalize the light curves from each sector.
The bottom left panels of Figures 2 and 3 plot Gaia DR2 color (GBP − GRP) versus Prot for our sample. The majority of the stars follow a common sequence, indicating that they are coeval.
2.3. A Gyrochronological Age
Gyrochronology only requires as input the mass of a star (or a proxy like temperature or color) and its Prot. There are a variety of empirical gyrochronology models available, including those of Barnes (2003, 2007) and its various recalibrations (e.g., Mamajek & Hillenbrand 2008; Angus et al. 2015; Barnes 2010). There are also theoretical models that pair stellar evolution with a magnetic torque law to predict angular momentum evolution (e.g., van Saders & Pinsonneault 2013; Gallet & Bouvier 2015; Matt et al. 2015). However, no model has been published that can explain all of the cluster rotation data (see Agüeros et al. 2018; Curtis et al. 2019; Douglas et al. 2019). Instead, we suggest that the best way to constrain the age of the Psc–Eri stream with gyrochronology is by comparing its Prot distribution directly to the distributions measured for benchmark clusters.
2.3.1. The Benchmark Cluster Sample
The Pleiades is ≈120 Myr old (Stauffer et al. 1998; see also Table 1), has a metallicity of [Fe/H] = +0.03 dex (Soderblom et al. 2009), and an interstellar reddening of E(B − V) ≈ 0.044 (AV = 0.14; Taylor 2006). Prot for 759 members were measured by Rebull et al. (2016a) from K2 light curves collected during its Campaign 4 (see also Rebull et al. 2016b; Stauffer et al. 2016). We cross-matched this list with Gaia DR2 and filtered out stars that were more than 0.375 mag discrepant from the single-star sequence, which we defined with the Gaia Collaboration et al. (2018b) membership list; this is half of the offset for an equal-mass binary (e.g., Hodgkin et al. 1999). We also removed stars with absolute differences in proper motion relative to the cluster median greater than 3 mas yr−1, corresponding to ≈2 km s−1 at 136 pc, or four times the internal velocity dispersion (Madsen et al. 2002).
Praesepe is 670 Myr old (Douglas et al. 2019) and has a metallicity of [Fe/H] = +0.15 dex (Cummings et al. 2017). Prot for 743 members were amassed from the literature and measured from K2 Campaign 5 light curves by Douglas et al. (2017). Douglas et al. (2019) cross-matched this list with DR2 and filtered out stars that failed membership, multiplicity, and data quality criteria, leaving us with 359 single-star members.
The 1-Gyr-old NGC 6811 cluster has a solar metallicity (Sandquist et al. 2016). Prot for 171 likely single-star members were recently measured by Curtis et al. (2019), more than doubling the size of the rotator sample from Meibom et al. (2011a) and extending its lower mass limit from ≈0.8 M⊙ to ≈0.6 M⊙.
2.3.2. Stellar Properties
Gaia DR2 provided effective temperatures (Teff) for ≈1.61 × 108 stars with 3000 ≲ Teff ≲ 10,000 K and G < 17 mag (Gaia Collaboration et al. 2018b) via the Apsis pipeline (Bailer-Jones et al. 2013). The DR2 photometry is very precise, but the Apsis temperatures are severely affected by interstellar reddening. However, this bias can be mitigated by dereddening the photometry for each cluster sample prior to converting it to Teff. We employ an empirical color–temperature relation to convert the dereddened Gaia DR2 (GBP − GRP)0 color to Teff. Our relation is a polynomial fit to benchmark stellar data assembled from the catalog of spectroscopic properties for the solar-type stars (4700 < Teff < 6700 K) targeted by the California Planet Survey (Brewer et al. 2016), warmer stars taken from the Hyades (Gaia Collaboration et al. 2018b) with Teff from the DR2/Apsis pipeline (Andrae et al. 2018), and cooler K and M dwarfs from the Boyajian et al. (2012) and Mann et al. (2015) catalogs. We have also applied this relation in Morris et al. (2018), Douglas et al. (2019), and Curtis et al. (2019).
2.3.3. The Psc–Eri Stream is Coeval with the Pleiades
In the left panel of Figure 4, we present the Prot distribution for likely single-star members of our three benchmark open clusters as a function of Teff. In the right panel, we add the Prot distribution for the Psc–Eri stream. The Prot distribution of the Psc–Eri stream is nearly indistinguishable from that of the Pleiades. In particular, the slow, converged sequences for each system are remarkably consistent.
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Standard image High-resolution imageThere are a few differences. The Psc–Eri stream has more outliers at periods intermediate to the slow sequence and the rapid ≈1 days rotators. This could be due to poor binary rejection, or slight differences in age—if younger than the Pleiades, those stars could still be converging. In addition, the Pleiades sample extends to much cooler Teff. As we discuss in Section 3.1, this is because RVs were used to identify members of the Psc–Eri stream, and DR2 does not provide RVs for such cool and faint stars. Finally, the warmest stars in the Psc–Eri stream (Teff ≳ 6100 K) appear to be rotating subtly and systematically faster than their analogs in the Pleiades. Perhaps this also indicates that the stream is slightly younger than the Pleiades.
In contrast, the late-F to early-K dwarfs are, again, remarkably consistent. The slow, converged sequences for both populations are well described by a line of constant Rossby number.10 Focusing on the stars with 4600 < Teff < 6100 K that have converged to within 25% of the slow sequence, the median and standard deviation of the Rossby number for the 43 Pleiades in this sample is Ro = 0.29 ± 0.03, and we find Ro = 0.29 ± 0.02 for the 39 stream members meeting the same criteria. These values are incredibly precise, and strikingly similar. The unavoidable conclusion is that the Psc–Eri stream is ≈120 Myr in age.11
3. Revisiting the Psc–Eri Stream's CMD
The left panel of Figure 5 is the CMD for the stream,12 together with members of the Pleiades (Gaia Collaboration et al. 2018b) and NGC 6811 (Curtis et al. 2019). We also include PARSEC isochrones (Bressan et al. 2012) appropriate for the Pleiades (130 Myr, solar metallicity) and NGC 6811 (1 Gyr, solar metallicity).
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Standard image High-resolution image3.1. The Apparent Absence of a Main-sequence Turnoff Is a Problem
The absence of Psc–Eri members warmer than Teff ≈ 7760 K on the main sequence would seem to favor an older age for the stream. However, as Meingast et al. (2019) pointed out, the stream lacks a clear main-sequence turnoff (MSTO). This is a problem: if the Psc–Eri stream is 1 Gyr old, there should be a well-defined MSTO (Figure 5 shows the case of NGC 6811). If the stream is young, the higher-mass stars should follow the Pleiades main sequence. Either way, these stars should exist somewhere in the CMD, but they are either missing from the stream or missing from its membership catalog.
Identifying members of most star clusters is facilitated by their spatial overdensity and distance from Earth: proper motions are sufficient and RVs are not strictly needed for finding candidate members. Identifying members of moving groups, stellar streams, and very nearby clusters (e.g., the Hyades) is more difficult because 3D kinematics are required. Accordingly, Meingast et al. (2019) used RVs to identify candidate Psc–Eri stream members. But the Gaia Radial Velocity Spectrometer (Soubiran et al. 2013; Cropper et al. 2018) provided measurements for stars with 3550 ≲ Teff ≲ 6900 K (Katz et al. 2019) in DR2. This data limitation means that the Meingast et al. (2019) criteria automatically precluded the identification of the MSTO for the Psc–Eri stream.
The left panel of Figure 5 plots the Pleiades membership (Gaia Collaboration et al. 2018b) and highlights those with DR2 RVs. The CMD for this Pleiades RV sample looks identical to the Meingast et al. (2019) membership for the Psc–Eri stream. We conclude that selecting members while requiring Gaia RVs will exclude warmer members, if they exist (as well as the coolest, lowest-mass stars and hot white dwarfs).
3.2. New, Massive Candidate Psc–Eri Members Support a Young Age
If the Psc–Eri stream is the same age as the Pleiades, we should be able to identify hotter, more massive stars that are spatially and kinematically consistent with the Meingast et al. (2019) members. To this end, we queried DR2 for stars with G < 10 mag, (GBP − GRP) < 0.5, and MG < 3 mag, which returned 435,601 stars. We trimmed this to 6851 stars by selecting those consistent with the stream in R.A. versus μαcos δ, R.A. versus , and decl. versus μδ diagrams. Next, we searched SIMBAD (Wenger et al. 2000) for RV measurements for these stars. We found 2332 matches for which we could then calculate 3D galactic UVW velocities.
Of these, 22 are within 5 km s−1 of the median value of the Meingast et al. (2019) members and within 20 pc of at least one member.13 While our velocity criterion is less restrictive than the 1.3 km s−1 velocity dispersion found by Meingast et al. (2019), our larger threshold is justified by the fact that hotter, rapidly rotating stars will have less precise RVs than those for the FGK dwarfs reported in DR2.14
Table 2. Rotation Periods for Meingast et al. (2019) Members of the Psc–Eri stream
# | Gaia DR2 Source ID | R.A. | Decl. | (GBP − GRP) | Teff | G | MG | Prot | Notes |
---|---|---|---|---|---|---|---|---|---|
(h:m:s) | (d:m:s) | (mag) | (K) | (mag) | (mag) | (day) | |||
1 | 3198972700981234048 | 04:22:31.5 | −07:33:03.2 | 0.432 | 7187 | 8.903 | 2.802 | 0.52 | Warm |
2 | 5181474045115843072 | 03:10:47.3 | −06:34:29.8 | 0.446 | 7161 | 8.562 | 2.954 | 0.87 | Warm |
3 | 2516948215250061568 | 02:20:22.6 | +05:52:59.1 | 0.597 | 6622 | 9.183 | 3.534 | 0.82 | Warm |
4 | 3245408684793798528 | 04:02:15.4 | −05:53:48.2 | 0.604 | 6573 | 9.425 | 3.513 | 0.56 | Conv. |
5 | 6628071944405827712 | 22:36:31.1 | −21:35:06.0 | 0.647 | 6320 | 8.967 | 3.835 | 0.94 | Conv. |
6 | 2988966044497883392 | 05:22:51.9 | −11:47:47.8 | 0.648 | 6487 | 10.345 | 3.688 | 0.79 | Conv. |
7 | 2456987757379368064 | 01:32:34.4 | −12:51:09.7 | 0.654 | 6259 | 9.043 | 3.865 | 1.24 | Conv. |
8 | 3186195241994234880 | 04:43:02.6 | −07:53:54.5 | 0.655 | 6206 | 9.999 | 3.766 | 1.71 | Conv. |
9 | 2988096919213031808 | 05:02:35.2 | −12:31:20.4 | 0.661 | 6387 | 10.280 | 3.869 | 0.91 | Conv. |
10 | 2987729922847457280 | 05:07:09.2 | −13:34:07.7 | 0.668 | 6240 | 10.156 | 3.896 | 0.97 | Conv. |
11 | 3204844780267292288 | 04:29:21.6 | −02:49:47.1 | 0.673 | 6173 | 9.760 | 4.020 | 1.97 | Conv. |
12 | 2405544971274027904 | 23:21:22.3 | −17:30:58.5 | 0.680 | 6139 | 9.222 | 4.024 | 1.44 | Conv. |
13 | 3190206672727634816 | 04:01:28.8 | −11:19:25.7 | 0.682 | 6324 | 9.920 | 4.059 | 2.26 | Conv. |
14 | 5182223980765557248 | 03:18:22.8 | −04:29:29.0 | 0.687 | 6105 | 9.788 | 4.054 | 1.29 | Conv. |
15 | 2982998926174605824 | 05:10:30.1 | −16:08:04.1 | 0.691 | 6081 | 10.646 | 3.970 | 1.70 | Conv. |
16 | 2492898356897645184 | 02:18:04.2 | −03:50:14.4 | 0.700 | 6075 | 9.453 | 4.126 | 2.67 | Conv. |
17 | 3256702490277205376 | 04:03:24.9 | −00:46:45.2 | 0.701 | 6033 | 9.928 | 4.180 | 3.08 | Conv. |
18 | 5104477754084350464 | 03:15:18.8 | −17:56:36.4 | 0.731 | 5993 | 9.606 | 4.279 | 2.55 | Conv. |
19 | 5147686052794315904 | 02:02:10.9 | −16:34:03.4 | 0.746 | 5864 | 9.643 | 4.410 | 2.53 | Conv. |
20 | 3197608241410937216 | 04:32:01.8 | −08:53:13.7 | 0.758 | 6418 | 10.494 | 4.476 | 2.85 | Conv. |
21 | 2489889607752127360 | 02:18:43.9 | −04:00:56.0 | 0.759 | 6016 | 10.019 | 4.390 | 2.38 | Conv. |
22 | 2346216668164370432 | 00:54:13.5 | −22:53:07.8 | 0.764 | 5852 | 9.441 | 4.452 | 3.10 | Conv. |
23 | 5129126330877050240 | 02:46:34.6 | −18:54:17.5 | 0.766 | 5926 | 9.784 | 4.520 | 3.00 | Conv. |
24 | 5070969209513725568 | 02:38:36.5 | −25:15:07.6 | 0.775 | 5852 | 9.435 | 4.462 | 5.69 | Slow |
25 | 2493286445846897664 | 02:15:46.4 | −02:36:32.5 | 0.821 | 5761 | 9.916 | 4.813 | 3.84 | Conv. |
26 | 3197753548744455168 | 04:33:55.4 | −08:19:27.9 | 0.827 | 5648 | 10.892 | 4.799 | 3.96 | Conv. |
27 | 2513568007268649728 | 02:14:47.2 | +02:14:20.4 | 0.865 | 5617 | 10.473 | 5.025 | 4.30 | Conv. |
28 | 5179904664065847040 | 03:09:03.7 | −07:03:55.8 | 0.873 | 5621 | 10.382 | 4.979 | 4.78 | Conv. |
29 | 5168681021169216896 | 03:29:30.3 | −07:10:13.8 | 0.895 | 5478 | 10.827 | 5.204 | 5.32 | Conv. |
30 | 3253302456727341696 | 04:07:34.7 | −02:04:33.2 | 0.901 | 5519 | 10.982 | 5.112 | 4.83 | Conv. |
31 | 3176016268285396864 | 04:21:35.2 | −14:01:29.9 | 0.902 | 5455 | 11.335 | 5.263 | 5.11 | Conv. |
32 | 2531732317316926336 | 01:15:31.7 | −02:50:46.4 | 0.903 | 5567 | 10.841 | 5.210 | 4.87 | Conv. |
33 | 2495781619982992640 | 02:45:01.2 | −02:25:46.3 | 0.921 | 5782 | 10.780 | 5.304 | 5.00 | Conv. |
34 | 2968825259219765120 | 05:29:28.5 | −19:17:58.8 | 0.924 | 5635 | 12.032 | 5.264 | 5.21 | Conv. |
35a | 4844691297067063424 | 04:11:51.9 | −37:56:23.0 | 0.927 | 5530 | 10.750 | 5.280 | 5.02 | Conv. |
36 | 2496200774431287424 | 02:30:58.8 | −03:03:04.9 | 0.928 | 5448 | 10.415 | 5.328 | 5.45 | Conv. |
37 | 4980826504625538048 | 00:38:12.2 | −43:00:24.8 | 0.935 | 5580 | 10.317 | 5.401 | 5.24 | Conv. |
38 | 4842810376267950464 | 03:47:56.3 | −41:56:24.9 | 0.936 | 5355 | 10.762 | 5.383 | 5.70 | Conv. |
39 | 3198734278756825856 | 04:26:27.1 | −07:39:39.7 | 0.966 | 5310 | 11.469 | 5.445 | 8.35 | Slow |
40 | 5045955865443216640 | 03:00:46.9 | −37:08:01.5 | 0.976 | 5434 | 10.323 | 5.363 | 3.90 | Rapid |
41 | 3193528950192619648 | 03:57:04.0 | −10:14:00.9 | 0.994 | 5270 | 11.297 | 5.534 | 5.54 | Conv. |
42 | 3187547465200970368 | 04:46:12.3 | −07:32:24.4 | 0.997 | 5425 | 11.733 | 5.519 | 5.43 | Conv. |
43 | 3245140743257978496 | 03:54:01.0 | −06:14:14.6 | 1.017 | 5344 | 11.146 | 5.434 | 5.66 | Conv. |
44 | 3205573756476323328 | 04:23:54.6 | −02:33:43.4 | 1.029 | 5134 | 11.604 | 5.634 | 6.05 | Conv. |
45 | 3185678437170300800 | 04:34:42.8 | −08:57:18.5 | 1.052 | 5122 | 11.899 | 5.796 | 0.55 | Rapid |
46 | 5103353606523787008 | 03:18:03.8 | −19:44:14.2 | 1.058 | 5077 | 10.473 | 5.227 | 1.26 | Rapid |
47 | 3187477818011309568 | 04:47:58.2 | −07:49:25.2 | 1.059 | 5205 | 11.994 | 5.818 | 7.02 | Conv. |
48 | 3009905594911137664 | 05:26:30.0 | −12:01:21.1 | 1.073 | 5352 | 12.576 | 5.905 | 6.50 | Conv. |
49 | 5083255496041631616 | 03:57:35.1 | −24:28:42.1 | 1.077 | 5078 | 11.131 | 5.885 | 12.22 | Slow |
50 | 3243665031151732864 | 03:48:38.3 | −06:41:52.6 | 1.082 | 5063 | 11.460 | 5.953 | 6.84 | Conv. |
51 | 3192643431015406464 | 04:21:53.2 | −08:43:16.1 | 1.088 | 5003 | 11.752 | 5.873 | 6.84 | Conv. |
52 | 5029398079322118912 | 01:13:42.4 | −31:11:39.6 | 1.088 | 5003 | 10.804 | 5.959 | 6.64 | Conv. |
53 | 2596395760081700608 | 22:39:53.5 | −16:36:23.3 | 1.097 | 5065 | 11.508 | 5.994 | 6.97 | Conv. |
54 | 2979827384884386176 | 04:58:02.5 | −17:10:27.7 | 1.113 | 5032 | 12.317 | 6.033 | 6.34 | Conv. |
55 | 3196687812738993152 | 04:06:00.2 | −06:53:50.0 | 1.128 | 4982 | 11.842 | 6.073 | 7.02 | Conv. |
56 | 2491594263092190464 | 02:10:22.3 | −03:50:56.7 | 1.136 | 4944 | 11.533 | 6.153 | 2.26 | Rapid |
57 | 2402197409339616768 | 22:39:01.4 | −18:52:55.7 | 1.142 | 4921 | 11.219 | 6.155 | 7.80 | Conv. |
58 | 3013355999838366336 | 05:25:14.6 | −10:25:49.4 | 1.159 | 4908 | 12.806 | 6.185 | 7.11 | Conv. |
59 | 5096891158212909312 | 04:12:46.0 | −16:19:29.1 | 1.181 | 4907 | 11.994 | 6.187 | 3.68 | Rapid |
60 | 4871041608622321664 | 04:28:28.9 | −33:53:45.1 | 1.193 | 4924 | 11.630 | 6.037 | 6.50 | Rapid |
61 | 7324465427953664 | 03:05:14.1 | +06:08:53.5 | 1.197 | 4947 | 12.043 | 6.247 | 4.40 | Rapid |
62 | 5097262136011410944 | 03:58:54.7 | −17:05:53.2 | 1.199 | 4899 | 11.649 | 6.311 | 7.58 | Conv. |
63 | 2418664520110763520 | 23:49:55.1 | −15:43:42.0 | 1.213 | 4917 | 11.607 | 6.396 | 2.94 | Rapid |
64 | 5179037454333642240 | 02:39:10.9 | −05:32:22.4 | 1.215 | 4859 | 11.765 | 6.373 | 6.42 | Rapid |
65 | 2484875735945832704 | 01:24:24.7 | −03:16:39.0 | 1.222 | 4842 | 11.791 | 6.398 | 8.40 | Conv. |
66 | 2393862836322877952 | 23:40:37.5 | −18:11:37.9 | 1.239 | 4734 | 11.485 | 6.472 | 7.70 | Conv. |
67 | 2594993646533642496 | 22:31:13.9 | −17:04:52.4 | 1.242 | 4829 | 11.934 | 6.451 | 6.10 | Rapid |
68 | 3199896668704440064 | 04:38:55.5 | −06:40:25.0 | 1.242 | 4890 | 12.458 | 6.305 | 4.28 | Rapid |
69 | 5114686272872474880 | 03:47:25.8 | −12:32:30.9 | 1.247 | 5006 | 12.634 | 6.550 | 9.00 | Conv. |
70 | 2433715455609798784 | 23:36:52.1 | −11:25:01.7 | 1.249 | 4810 | 11.737 | 6.442 | 6.30 | Rapid |
71 | 5106733402188456320 | 03:24:25.2 | −15:50:05.4 | 1.278 | 4944 | 11.517 | 6.197 | 0.62 | Rapid |
72 | 2390974419276875776 | 23:48:32.4 | −18:32:57.4 | 1.283 | 4706 | 11.583 | 6.618 | 6.50 | Rapid |
73 | 3172630287868034944 | 04:26:48.2 | −15:25:47.4 | 1.307 | 4881 | 12.334 | 6.599 | 5.85 | LM |
74 | 5161117923061794688 | 02:59:52.0 | −09:47:35.8 | 1.308 | 4800 | 12.063 | 6.639 | 5.45 | LM |
75 | 5155187986271622912 | 03:20:33.3 | −14:16:58.4 | 1.320 | 4776 | 12.307 | 6.687 | 1.93 | LM |
76 | 5129876953722430208 | 02:29:28.5 | −20:12:16.8 | 1.334 | 4829 | 11.695 | 6.739 | 8.00 | LM |
77 | 2339984636258635136 | 23:56:53.7 | −23:17:24.6 | 1.349 | 4545 | 11.475 | 6.765 | 8.35 | LM |
78 | 3195826963854173056 | 04:06:29.4 | −07:35:32.2 | 1.366 | 4828 | 12.987 | 6.797 | 10.73 | Slow |
79 | 2349094158814399104 | 00:47:18.0 | −22:45:08.1 | 1.366 | 4585 | 10.929 | 6.051 | 1.30 | LM |
80 | 3247412647814482816 | 03:32:30.9 | −06:13:09.1 | 1.382 | 4714 | 12.327 | 6.898 | 6.66 | LM |
81 | 4975223840046231424 | 00:47:38.5 | −47:41:45.8 | 1.420 | 4551 | 11.514 | 6.985 | 5.80 | LM |
82 | 3191365111308746880 | 04:24:30.4 | −10:41:02.4 | 1.423 | 4719 | 12.901 | 6.944 | 7.02 | LM |
83 | 3197607794734344320 | 04:31:51.6 | −08:54:03.5 | 1.439 | 4440 | 13.133 | 7.059 | 8.02 | LM |
84 | 3171136944919260928 | 04:36:36.1 | −17:47:23.7 | 1.439 | 4469 | 12.879 | 6.940 | 7.85 | LM |
85 | 3206907086126334464 | 05:13:25.5 | −08:19:52.2 | 1.465 | 4364 | 13.320 | 7.086 | 6.66 | LM |
86 | 3177883999240571904 | 04:35:35.3 | −12:47:47.6 | 1.480 | 4512 | 12.828 | 6.356 | 4.00 | LM |
87 | 2488721720245150336 | 02:26:53.3 | −05:17:45.2 | 1.498 | 4444 | 12.485 | 7.198 | 5.20 | LM |
88 | 5159567164990031360 | 03:04:46.0 | −12:16:57.9 | 1.560 | 4330 | 12.613 | 7.098 | 0.45 | LM |
89 | 5081912751826042624 | 03:47:01.6 | −26:16:11.2 | 1.577 | 4410 | 12.968 | 7.389 | 4.50 | LM |
90 | 5118895478259982336 | 02:26:07.0 | −24:54:49.0 | 1.579 | 4431 | 11.728 | 6.658 | 5.61 | LM |
91 | 5117016378528360448 | 02:17:14.6 | −27:16:41.9 | 1.591 | 4308 | 12.551 | 7.451 | 5.92 | LM |
92 | 5149427640557882368 | 02:02:58.3 | −13:37:46.8 | 1.594 | 4207 | 11.982 | 7.442 | 11.96 | Slow |
93 | 4832163770817481856 | 03:58:17.4 | −46:34:13.0 | 1.630 | 4261 | 12.992 | 7.559 | 7.80 | LM |
94 | 2531488844210764544 | 01:08:57.0 | −03:01:31.9 | 1.661 | 4168 | 13.074 | 7.612 | 2.26 | LM |
95 | 2480756793589426944 | 01:33:49.3 | −04:28:41.7 | 1.670 | 4228 | 13.216 | 7.682 | 6.50 | LM |
96 | 2355466790769878400 | 00:55:21.5 | −21:24:03.7 | 1.689 | 4135 | 12.341 | 7.578 | 6.84 | LM |
97 | 5114516020369038848 | 03:51:15.9 | −12:23:46.4 | 1.732 | 4298 | 13.375 | 7.484 | 0.68 | LM |
98 | 5068272932125221504 | 02:26:04.6 | −29:23:48.9 | 1.768 | 4163 | 12.815 | 8.000 | 7.80 | LM |
99 | 5094664333632217088 | 04:02:18.0 | −18:42:45.4 | 1.771 | 4076 | 12.631 | 7.134 | 2.62 | LM |
100 | 5121805541941481472 | 01:57:17.2 | −25:13:49.6 | 1.784 | 3956 | 12.793 | 7.931 | 5.45 | LM |
101 | 4984094970441940864 | 01:21:49.7 | −42:01:22.3 | 1.852 | 4113 | 12.731 | 8.099 | 5.45 | LM |
Notes. Columns: # is the row number sorted by (GBP − GRP); R.A., decl., (GBP − GRP) Teff, G, and MG = G − 5 log10 (100/π) are from Gaia DR2; Prot is measured from TESS FFI data (days). The notes indicate if a star is converged on the slow sequence (Conv.), slower than the converged sequence (Slow), more rapid than the converged sequence (Rapid), has a lower mass (LM) than the converged sequence limit, or is too warm to efficiently spin down (Warm). Regarding the "Slow" stars, five stars appear to rotate more slowly than the bulk of the sample. Blending is not a concern for these stars (i.e., none have bright neighbors in DR2 within 15), their spot-modulated light curves show unambiguous periodicity, and they do not appear to be binaries according to their photometry, RV errors (σ < 2 km s−1), and kinematics. It is unclear to us why they are outliers.
aThis star has been identified as a planet candidate host by TESS (TOI 451, TIC 257605131) and appears to show two sets of transits with periods of 9.19 days and 16.36 days, which await validation.A machine-readable version of the table is available.
We also searched the 10 pc volume around every Meingast et al. (2019) member for comoving neighbors, according to the proper motion criterion Δμ < 2 mas yr−1, and found 377 comoving candidates, including 10 high-mass stars. Oh et al. (2017) performed a similar exercise to identify comoving pairs and larger groups using a more sophisticated algorithm applied to the Tycho–Gaia Astrometric Solution (TGAS; Michalik et al. 2015) catalog, released with Gaia DR1 (see also Andrews et al. 2017). While the Psc–Eri stream was not identified as a comoving system in their analysis, they did identify seven high-mass stars as comoving partners with members from Meingast et al. (2019), adding two unique stars to our high-mass candidate list (12 comoving neighbors in total). Table 3 lists our 34 high-mass candidate members.
Table 3. Candidate Massive Members of the Psc–Eri stream
# | Gaia DR2 ID | α(ICRS) | δ(ICRS) | GBP − GRP | G | MG | RV | Δv | Δμ | Δr | Name |
---|---|---|---|---|---|---|---|---|---|---|---|
(h:m:s) | (d:m:s) | (mag) | (mag) | (mag) | (km s−1) | (km s−1) | (mas yr−1) | (pc) | |||
1 | 3305012316783145728 | 04:00:40.81 | +12:29:25.0 | −0.008 | 3.387 | −2.039 | 17.8 | 1.3 | 2.3 | 18.7 | λ Taua |
2 | 2676509823708845056 | 22:03:18.87 | −02:09:19.5 | −0.083 | 4.622 | −1.178 | 11.0 | 3.4 | 1.1 | 17.7 | o Aqrb |
3 | 5021010046848175616 | 02:04:29.45 | −29:17:48.3 | −0.193 | 4.638 | −0.447 | 18.5 | 4.1 | 5.8 | 6.3 | ν Forc |
4 | 2391220091406075648 | 23:44:12.11 | −18:16:37.1 | −0.080 | 5.185 | −0.102 | 16.0 | 1.8 | 3.0 | 6.9 | 106 Aqr |
5 | 2390144081839340288 | 23:51:21.37 | −18:54:33.1 | −0.153 | 5.125 | 0.096 | 12.7 | 2.9 | 0.3 | 0.9 | 108 Aqrd |
6 | 2597327566122330880 | 22:47:42.80 | −14:03:23.3 | −0.037 | 5.666 | 0.481 | 15.0 | 3.9 | 1.2 | 11.4 | τ1 Aqr |
7 | 2734781844037454592 | 22:24:00.51 | +15:16:53.1 | −0.085 | 6.764 | 0.503 | 5.0 | 2.8 | 0.9 | 14.6 | HD 212442 |
8 | 2428341184508675456 | 00:14:54.54 | −09:34:10.6 | −0.103 | 5.747 | 0.531 | 19.9 | 3.9 | 0.7 | 11.8 | HR 51 |
9 | 4878579825983429248 | 04:36:50.91 | −30:43:00.3 | −0.100 | 6.252 | 0.569 | 14.5 | 4.1 | 2.3 | 10.2 | HR 1476 |
10 | 2746298781663140352 | 23:55:07.82 | +07:04:15.2 | −0.074 | 6.196 | 0.762 | 16.8 | 4.1 | 2.4 | 4.5 | 26 Psc |
11 | 6549670305714644608 | 23:06:53.67 | −38:53:32.2 | 0.054 | 5.631 | 0.921 | 11.9 | 3.1 | 2.0 | 17.5 | υ Grue |
12 | 5045432364765457792 | 02:57:32.63 | −38:11:27.2 | −0.022 | 6.395 | 1.062 | 19.6 | 2.0 | 1.7 | 18.6 | HR 893 |
13 | 2410222091875449216 | 23:09:49.58 | −14:30:38.1 | 0.033 | 6.411 | 1.276 | 16.6 | 3.3 | 0.9 | 7.5 | HR 8816 |
14 | 3252923090855768064 | 04:04:53.38 | −02:25:37.8 | −0.007 | 7.056 | 1.353 | ⋯ | ⋯ | 1.4 | 5.1 | HD 25752 |
15 | 5175455696422545664 | 02:35:24.47 | −09:21:02.8 | 0.016 | 7.097 | 1.445 | 19.1 | 1.6 | 3.4 | 8.8 | HD 16152 |
16 | 3192744139408470272 | 04:21:35.19 | −08:06:31.1 | 0.022 | 7.483 | 1.537 | ⋯ | ⋯ | 1.5 | 5.0 | HD 27665 |
17 | 2982108287397220992 | 05:23:07.86 | −17:13:26.1 | 0.064 | 8.250 | 1.567 | ⋯ | ⋯ | 0.7 | 6.2 | HD 35308 |
18 | 2741090498161113344 | 00:15:57.32 | +04:15:03.8 | 0.052 | 7.107 | 1.607 | 12.6 | 2.1 | 1.3 | 6.2 | HD 1160 Af |
19 | 2697317256631380736 | 21:58:36.60 | +06:00:49.8 | 0.083 | 7.964 | 1.679 | ⋯ | ⋯ | 1.5 | 4.6 | HD 208800 |
20 | 2721809496615333248 | 22:00:50.95 | +07:51:08.5 | 0.070 | 7.989 | 1.713 | ⋯ | ⋯ | 1.2 | 3.8 | HD 209105 |
21 | 2986248601510045184 | 05:00:01.23 | −15:47:55.2 | 0.060 | 8.372 | 1.732 | 14.9 | 4.7 | 1.1 | 6.6 | HD 32077 |
22 | 2542373597009506944 | 00:31:40.77 | −01:47:37.4 | 0.094 | 7.041 | 1.776 | ⋯ | ⋯ | 1.0 | 5.2 | HD 2830 |
23 | 2971453886581625600 | 05:36:04.99 | −16:51:45.1 | 0.105 | 8.561 | 1.783 | ⋯ | ⋯ | 0.8 | 11.5 | HD 37190 |
24 | 2391000395239148672 | 23:52:39.91 | −18:33:42.8 | 0.122 | 6.804 | 1.806 | 13.0 | 2.9 | 0.9 | 0.1 | HD 223785 |
25 | 5127759431765387392 | 02:45:18.39 | −20:24:05.9 | 0.058 | 7.106 | 1.827 | ⋯ | ⋯ | 0.3 | 3.1 | HD 17224 |
26 | 2982652206352410624 | 05:12:33.00 | −17:27:16.5 | 0.117 | 8.514 | 1.899 | ⋯ | ⋯ | 1.8 | 6.2 | HIP 2427 |
27 | 2982652275071888128 | 05:12:29.72 | −17:27:08.9 | 0.119 | 8.564 | 1.961 | ⋯ | ⋯ | 0.7 | 6.7 | HD 33857 |
28 | 3182650382147268992 | 05:07:44.10 | −09:51:53.5 | 0.212 | 8.717 | 2.137 | 13.9 | 3.5 | 0.5 | 13.3 | HD 33126e |
29 | 5145324782854148096 | 02:13:19.11 | −14:54:27.3 | 0.495 | 7.556 | 2.226 | 19.0 | 3.1 | 9.3 | 8.1 | HD 13722 |
30 | 3185719600136840064 | 04:35:06.82 | −08:41:36.6 | 0.273 | 8.538 | 2.327 | ⋯ | ⋯ | 1.3 | 6.7 | HD 29152 |
31 | 3300937801567693824 | 04:15:00.92 | +10:44:53.1 | 0.283 | 7.652 | 2.385 | 16.0 | 2.1 | 3.1 | 18.6 | HD 26843 |
32 | 2736194815262723712 | 22:34:06.27 | +16:01:27.2 | 0.318 | 8.886 | 2.549 | 8.2 | 2.5 | 0.4 | 14.7 | HD 213838 |
33 | 5155416822128110208 | 03:18:13.96 | −13:49:45.4 | 0.303 | 8.226 | 2.625 | ⋯ | ⋯ | 1.7 | 2.0 | HD 20573 |
34 | 3175513589608066048 | 04:19:34.07 | −15:10:11.8 | 0.415 | 8.999 | 2.927 | 19.5 | 2.6 | 2.8 | 3.6 | HD 27467e |
Notes. Columns—# is the row number, sorted by MG; α(ICRS, epoch 2015.5), δ(ICRS, epoch 2015.5), (GBP − GRP), G, and MG = G − 5 log10 (100/ϖ) from Gaia DR2; RV obtained from SIMBAD; Δv is the absolute deviation of UVW velocities from the stream's median value (km s−1); Δμ is minimum difference in proper motion relative to the nearest neighbor in the Meingast et al. (2019) list (mas yr−1); ΔXYZ: the physical distance (parsec) to the nearest Meingast et al. (2019) member; common aliases. Notes on particular stars from SIMBAD are provided below.
aAlgol-type EB. bBe star. cα2 CVn variable. dPeculiar composition. eBinary or multiple star. fHD 1160 has two low-mass companions (Nielsen et al. 2012)—HD 1160 C is an M3.5 dwarf (Gaia DR2 2741090498159705216) and HD 1160 B is a brown dwarf candidate with an estimated mass of 39–166 MJup (Maire et al. 2016), 35–90 MJup, and 70–90 MJup (Garcia et al. 2017), depending on the age of the host star. Interpolating the 125 ± 15 Myr evolutionary models from Baraffe et al. (2015) at the Garcia et al. (2017) temperature (Teff = 3050 ± 50 K) and luminosity, corrected with the Gaia DR2 parallax (log L/L⊙ = −2.59 ± 0.05 dex), we infer a mass of MB = 0.12 ± 0.01 M⊙(≈123 MJup). This is greater than the hydrogen-burning limit and indicates that HD 1160 B is probably a very-low-mass star and not a brown dwarf.A machine-readable version of the table is available.
Download table as: DataTypeset image
The right panel of Figure 5 shows the CMD for the Pleiades members together with the Meingast et al. (2019) Psc–Eri stream members and our high-mass candidate members. The Pleiades has 239 members with DR2 RVs (Gaia Collaboration et al. 2018b), and Meingast et al. (2019) identified 256 members of the Psc–Eri stream. The sizes of these samples are approximately equal, so we expect that the Psc–Eri stream should have a similar number of higher-mass stars, and perhaps a similar population size and total mass.15 The Pleiades list has 43 more that are brighter and warmer than the Teff ≈ 7000 K RV cutoff, and we found 34 candidates in the stream.
Two of the five brightest candidates in the CMD are expected to have atypical photometry and should be excluded from an isochronal age analysis (Cummings & Kalirai 2018): according to SIMBAD, λ Tau is an Algol-type eclipsing binary and omi Aqr is a Be star. Focusing on the blue edge of the upper main sequence, the Psc–Eri strea appears approximately coeval with the Pleiades. The 80 and 130 Myr PARSEC isochrones shown in the right panel of Figure 5 do not diverge appreciably in color at the luminosities covered by the Pleiades and Psc–Eri stream samples. We postpone a precise isochronal analysis until we can validate the membership of our high-mass candidates with new RV measurements.
3.3. How Did the Psc–Eri Stream Form?
Meingast et al. (2019) estimated the Psc–Eri stream progenitor cluster mass to be ≈2000 M⊙, noted that the Hyades initial mass has been estimated to be ≈1700 M⊙, and concluded that since the Hyades still has a gravitationally bound core, the Psc–Eri stream, which has been dispersed, must be older.
Indeed, if it were truly 1 Gyr old, the Psc–Eri stream would have had to be born as a dense cluster analogous to the Pleiades, Hyades, or NGC 6811 to survive for so long before disrupting. However, given that we now know that it is actually ≈120 Myr, this constraint on the stream's birth conditions is unnecessary. In their figure A.1 and table A.2, Meingast et al. (2019) identified four main clumps within the stream. These clumps are presently separated by ≈160 pc, and this clumpiness is similar to that seen in the much younger Tuc–Hor (Kraus et al. 2014) or Sco–Cen associations (Preibisch & Mamajek 2008; Pecaut & Mamajek 2016; Wright & Mamajek 2018), which are gravitationally unbound.
We suggest that the members of the Psc–Eri stream were not formed in a dense cluster but instead formed in a more decentralized fashion, similar to these OB associations. If correct, this would resolve the following two challenges to our young age result.
- 1.Why does the stream not have a well-defined core? Our answer is that it never had one, but instead formed several smaller clumps.
- 2.How could a 120-My-old cluster disperse its stars across 400 pc with such a low internal velocity dispersion? The ends of the stream had a head start, as they were born separated in space, and the members of each subgroup dispersed from there.
According to the Gaia Collaboration et al. (2018b) membership lists, the Pleiades has 611 members within 5 pc of its center, and the Hyades has 195 members in the same size volume. In contrast, we suggest that the stream formed multiple approximately coeval clumps; therefore, each zero-age core density is much less than expected based on the present-day star count.
If we are correct, this would mean that the stream provides an environment to its stars that is distinct from that of the Pleiades, and which might be representative of a more common star formation channel in the Galaxy than dense cluster formation (e.g., Clark et al. 2005). That would make the Psc–Eri stream an excellent target for exoplanet searches, which have so far turned up nothing for the Pleiades (Gaidos et al. 2017).
4. Conclusion
Meingast et al. (2019) discovered an exciting new stellar stream located relatively nearby (d ≃ 80–226 pc). We were intrigued by its apparently old age (≈1 Gyr), as this would make it a critical target for the calibration and validation of a variety of age-dating techniques, including stellar activity, rotation, lithium depletion, and other chemical clock techniques.
Using new time-series photometry from TESS, we measured Prot for 101 of the Psc–Eri stream's members. We found that the majority of these members actually overlap with the Prot distribution for the Pleaides, indicating that the Psc–Eri stream is only ≈120 Myr old.
By contrast to the CMD for the ≈1 Gyr old cluster NGC 6811, the Meingast et al. (2019) CMD for the Psc–Eri stream lacked an MSTO. We concluded that this is because the Psc–Eri stream is young, and that the more massive stars that would otherwise occupy the MSTO are warmer than the Teff ≲ 7000 K cutoff for the Gaia DR2 RV data set, i.e., warmer stars could not be detected in DR2 as members by Meingast et al. (2019) because they lack 3D kinematics. We expanded the search for these missing members by pairing DR2 with RV measurements in the literature tabulated by SIMBAD, and also by searching for comoving neighbors to the known members. We found 34 candidates that closely track the upper main sequence of the Pleiades, further strengthening our finding of a young age for the Psc–Eri stream.
There is one point on the Psc–Eri stream's CMD consistent with an old age: the evolved 42 Cet triple system. Given the indisputably young age for the Psc–Eri stream we found with gyrochronology, we suspect it is an interloper.
Meingast et al. (2019) estimated that the stream was formed with a total stellar mass similar to the Hyades. The Hyades has retained a dense cluster structure (with tidal tails; Meingast & Alves 2019), as has the Pleiades, while the stream is diffuse, with an elongated structure spanning 400 pc with four clumps. We argued that rather than being evidence for an older age, this structure indicates that the Psc–Eri stream's stars did not form in a dense cluster environment, but instead in the more decentralized fashion typical of OB associations.
If true, the Psc–Eri stream could become a valuable benchmark system for comparing environmental impact relative to the Pleiades, and for examining how photoevaporation sculpts planet sizes. To date, no planets have been found in the Pleiades (Gaidos et al. 2017). The stream thus presents a new opportunity to search for Pleiades-aged planets. Indeed, a Psc–Eri member has already been identified as a planet candidate host with TESS.16
This is the first gyrochronology study using TESS data, and it confirms that TESS will be an exciting mission for stellar astrophysics. This is especially true given how TESS records and releases FFI data. The existence of this stream was not known prior to the TESS Cycle 1 call for proposals, and yet the FFI data were ready for us to analyze immediately following the announcement of the stream's discovery by Meingast et al. (2019). This is also the first time a stellar stream has been age-dated using gyrochronology, and our work demonstrates the potential for gyrochronology to serve as a powerful tool for Galactic archeology.
We thank Stefan Meingast for kindly providing us with the Meingast et al. (2019) membership list prior to its posting to the CDS, and Tim White for helpful discussions about 42 Ceti. The association of TOI 451 with Psc–Eri was first noted by Elisabeth Newton; we thank her and the THYME collaboration, including Aaron Rizzuto, Andrew Vanderburg, Andrew Mann, and Benjamin Tofflemire, and Adam Kraus for discussing this exciting planet candidate with us.
J.L.C. is supported by the National Science Foundation Astronomy and Astrophysics Postdoctoral Fellowship under award AST-1602662.
Part of this research was carried out at the Jet Propulsion Laboratory, California Institute of Technology, under a contract with NASA.
The Center for Exoplanets and Habitable Worlds is supported by the Pennsylvania State University, the Eberly College of Science, and the Pennsylvania Space Grant Consortium.
This work has made use of data from the European Space Agency (ESA) mission Gaia,17 processed by the Gaia Data Processing and Analysis Consortium (DPAC).18 Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement.
This research made use of NASA's Astrophysics Data System, and the VizieR and SIMBAD (Wenger et al. 2000) databases, operated at CDS, Strasbourg, France.
Facilities: TESS - , Gaia - .
Software: The IDL Astronomy User's Library (Landsman 1993),19 TESScut (i.e., Astrocut; Brasseur et al. 2019).20
Footnotes
- 7
The stream was undesignated in Meingast et al. (2019). The authors of the discovery paper suggested the name "MAF-1" for the stream (S. Meingast 2019, private communication), however, this is very different from the nomenclature for nearby associations (e.g., de Zeeuw et al. 1999; Torres et al. 2008). This acronym could be confused with two acronyms already in the Dictionary of Nomenclature of Celestial Objects (http://cds.u-strasbg.fr/cgi-bin/Dic-Simbad; Lortet et al. 1994)—[MAF2004] and [MAF2009]—the latter of which is used for members of the open cluster NGC 7062 (Molenda-Żakowicz et al. 2009), or as an abbreviation of the Maffei galaxies or Maffei Group of galaxies (e.g., Fingerhut et al. 2007). Two of the main concentrations of the stream's members are in the constellations Eridanus (clump 1) and Pisces (clump 3), and the group's convergent point (α, δ ≃ 426, −200; ICRS) lies in Eridanus as well. As we find in our analysis that the group is more analogous to an older version of an OB association, similar to other expansive nearby stellar associations like Sco–Cen and Tuc–Hor, we combine the two prominent constellation names and refer to it as the Pisces–Eridanus stream or Psc–Eri.
- 8
- 9
- 10
Ro = Prot/τ. We used the formula for convective turnover time, τ, from Cranmer & Saar (2011).
- 11
We performed similar comparisons with M35 (NGC 2168, 150 Myr; Meibom et al. 2009) and M34 (NGC 1039, 220 Myr; Meibom et al. 2011b), and found that the Psc–Eri Prot distribution was most consistent with that of the Pleiades. Specifically, the slow sequences for the older M35 and M34 clusters are converged to lower masses and longer periods (see Figure 12 in Stauffer et al. 2016), whereas the slow sequences for Psc–Eri and the Pleiades share a common maximum Prot of ≈8.5 days, where the distributions turn over toward more rapid rotation toward lower masses and cooler temperatures.
- 12
We adopt d = 1000/ϖ to estimate distances for each star, and so calculate absolute magnitudes as MG = G − 5 log10 (100/ϖ), with units of parsec and mas for d and ϖ.
- 13
The median and maximum separation between nearest neighbors in the Meingast et al. (2019) membership list is 9 and 26 pc; the median and maximum velocity deviations from the stream's average UVW velocity are 3 and 6 km s−1.
- 14
Restricting the velocity criterion to ≤3 km s−1 reduces the candidate list from 22 to 11 stars. Similarly, only 55% of the Meingast et al. (2019) list has Δv ≤ 3 km s−1 in Cartesian UVW velocities.
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First noted by Elisabeth Newton as a Psc–Eri member (private communication), TOI 451 is a G dwarf with Teff ≈ 5530 K (Gaia DR2 4844691297067063424, CD−38 1467, TIC 257605131). Our analysis of the TESS two-minute light curves from Sectors 4 and 5 reveals two sets of transits, suggesting that TOI 451 hosts two planets with Porb,b ≈ 9.19 days and Porb,c ≈ 16.36 days. Follow-up efforts to rule out false-positive scenarios and validate the planetary system are being coordinated by the TESS Hunt for Young Moving group Exoplanets collaboration (THYME).
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