arxiv: 2604.13983 · v1 · submitted 2026-04-15 · 🌌 astro-ph.SR

Recognition: unknown

Radial Velocity Evidence for a Post-Mass-Transfer Massive Binary System: NaSt1

Adriana Kuehnel, Bradford P. Holden, Jared A. Goldberg, Jonathan Swift, Kishalay De, Kittipong Wangnok, Kyle W. Davis, Nathan Smith, Poemwai Chainakun, R. Paul Butler, Ryan J. Foley, Ryan M. Lau, Samaporn Tinyanont, Steven S. Vogt

Authors on Pith no claims yet

Pith reviewed 2026-05-10 12:00 UTC · model grok-4.3

classification 🌌 astro-ph.SR

keywords NaSt1binary starsradial velocityemission linesmassive starsstellar windsmass transfersupernova progenitors

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The pith

Detection of opposing radial velocity variations in NaSt1's emission lines establishes it as a massive binary system after mass transfer.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The authors use high-resolution spectroscopy to measure radial velocities in NaSt1 and find periodic variations in two distinct sets of 35 emission lines. These sets vary with the same 310-day period but in opposite phases, which the paper links to the wind from a stripped primary star and the region where that wind collides with the companion's wind. This evidence supports the idea that NaSt1 is a binary system that has already undergone significant mass transfer. Supporting photometry and spectroscopy show matching periods, two dust components, and a young expanding nebula. Such a system offers a nearby example of how massive stars can lose their outer layers before becoming stripped-envelope supernovae.

Core claim

Multi-epoch high-resolution optical spectroscopy of NaSt1 reveals two groups of 35 emission lines that exhibit radial velocity variations with a period of 310 ± 6 days but in opposing phases. These are interpreted as originating from the optically thick wind of the stripped primary star and the wind-wind collision region with its companion, offering strong evidence for the system's binary nature. The period matches the light curve period, inconsistent with pulsations or ellipsoidal modulation, while modeling shows hot and warm dust and an expanding nebula with a dynamical age of about 40 years.

What carries the argument

The radial velocity curves of two opposing-phase groups of emission lines, associated with the primary star's wind and the wind-collision zone.

If this is right

The consistent RV and light curve periods exclude ellipsoidal modulation as the cause of variability.
The phase relationship rules out stellar pulsations in favor of a binary interpretation.
Modeling of the infrared spectrum identifies two optically thin dust components at different temperatures.
Spatially resolved spectroscopy shows a circumstellar nebula expanding at 31 km/s with a dynamical age of roughly 40 years.
The system serves as a Galactic example of a massive binary in the process of becoming a stripped-envelope supernova progenitor.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

If the line identifications hold, similar RV monitoring of other emission-line objects could uncover additional post-mass-transfer binaries.
The short dynamical age of the nebula implies that the mass-loss episode is recent, which could be tested by searching for changes in the nebula's size or brightness over the next decade.
Confirmation of this binary channel would help calibrate models of envelope stripping in massive stars leading to supernovae.

Load-bearing premise

The two groups of emission lines must originate from the primary's wind and the wind-collision region specifically, and the observed period must be the orbital period rather than a harmonic or unrelated cycle.

What would settle it

Future observations that fail to show the 310-day periodicity persisting in the radial velocities of the two line groups or that show the phases no longer opposing each other would falsify the binary interpretation.

Figures

Figures reproduced from arXiv: 2604.13983 by Adriana Kuehnel, Bradford P. Holden, Jared A. Goldberg, Jonathan Swift, Kishalay De, Kittipong Wangnok, Kyle W. Davis, Nathan Smith, Poemwai Chainakun, R. Paul Butler, Ryan J. Foley, Ryan M. Lau, Samaporn Tinyanont, Steven S. Vogt.

**Figure 1.** Figure 1: High-resolution He II λ4686 line profiles of NaSt1 from seven observing epochs between 2021 and 2022. The spectra are normalized to the continuum and corrected for barycentric motion. They are vertically offset for clarity. NaSt1 was recognized as a variable star with the reference ID ASASSN-V J185217.55+005944.3 in the Variable Star Database (T. Jayasinghe et al. 2020). The ATLAS project also provides t… view at source ↗

**Figure 2.** Figure 2: Multiband photometric light curves of NaSt1 in ZTF-g, ZTF-r, ASAS-SN-g, ASAS-SN-V , ATLAS-c, ATLAS-o, and PGIR-J. Open symbols denote photometry reported in R. M. Lau et al. (2021), while filled symbols represent archival data analyzed in this work. the paper; MJD 59386). Observations of an A0V star were obtained close in airmass and time to provide telluric correction. We obtained spectra using the 0. ′′… view at source ↗

**Figure 3.** Figure 3: RV variations with respect to the first epoch for 35 emission lines in NaSt1 derived from the CCF analysis. Panels (a), (b), and (c) show representative lines associated with the wind–wind collision (WWC) region, the inner circumbinary material (ICM), and the outer circumbinary material (OCM), respectively (see Section 4.2). The highest ionization lines in panel (a) exhibit a phase offset relative to those… view at source ↗

**Figure 4.** Figure 4: Time-domain LCs and RVs of NaSt1. The top panels show ZTF-r and ATLAS-o photometry, and the lower panels present RVs measured from He He II λ4686, He I λ6678, [Ca VII] λ5618, and [Fe VII] λ6087. Open symbols denote photometry previously reported by R. M. Lau et al. (2021), while filled symbols represent new observations presented in this work. Solid curves show the best-fitting sinusoidal models with a per… view at source ↗

**Figure 5.** Figure 5: Mid-IR spectrum of NaSt1 and the best-fitting two-component dust model, comprising hot and warm dust components constrained by MCMC fitting (top panel). The bottom panel shows the modeled optical depth, which remains below τ ∼ 0.03 across 1–5 µm and decreases toward longer wavelengths, consistent with optically thin emission. 4.2. Line-forming regions The emission-line spectrum of NaSt1 indicates contrib… view at source ↗

**Figure 6.** Figure 6: (a) Continuum (blue) and [N II] λ6584 emission (red) along the projected major (black) and minor (green) axes. Contours are shown at 0.1, 0.5, and 0.9 of their respective peak intensities. (b) Radial velocity (RV) map of the [N II] emission, with the same projected axes overplotted. The blue contour indicates the 0.5 continuum level, representing the point spread function (PSF) of an unresolved source. (c)… view at source ↗

**Figure 7.** Figure 7: Schematic illustration of the proposed circumstellar configuration of NaSt1. The stripped star drives a strong stellar wind, while the less massive companion produces a weaker wind, forming a wind–wind collision (WWC) region between the two stars. The blue region represents the inner circumbinary material (ICM), and the green region indicates the outer circumbinary material (OCM). Example emission-line pro… view at source ↗

read the original abstract

We present multi-epoch high-resolution optical spectroscopy ($R \simeq 80{,}000$) of the emission-line object NaSt1 to test its proposed binary nature, along with long-term multiband photometry, mid-infrared spectroscopy, and spatially resolved integral field unit (IFU) spectroscopy to probe the circumstellar kinematics of the system. We detect two groups of 35 emission lines showing radial velocities (RVs) variation of the same period of 310 $\pm$ 6 d, but with opposing phase, which we associate with the optically thick wind of the stripped primary star and the wind-wind collision region with the companion star, providing a strong evidence for binarity. The RV and light curve (LC) periods are consistent within the uncertainties, ruling out ellipsoidal modulation, which would require an orbital period of about 620 d. The phase relationship between the RV and LC is inconsistent with stellar pulsations and supports a binary origin. We model the 1--5~$\mu$m spectrum of NaSt1 and find two optically thin dust components: hot $T_{\rm h} \simeq 1230$ K, $M_{\rm h} \simeq 2 \times 10^{-10} M_{\odot}$ and warm $T_{\rm c} \simeq 660$ K, $M_{\rm c} \simeq 3 \times 10^{-8} M_{\odot}$. IFU spectroscopy spatially resolves the circumstellar medium in the [\ion{N}{2}] $\lambda6548$ and $\lambda6584$ emission lines, showing a deprojected expansion velocity of $\sim31$ km~s$^{-1}$, implying a dynamical age of $\sim40$ yr. This short timescale suggests that the nebula was produced by recent mass loss. The system may represent a Galactic analog of a massive binary undergoing a mass-loss process to become a stripped-envelope supernova progenitor.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Desk Editor's Note private letter to a colleague

NaSt1 shows a new 310-day RV period split across two opposing line groups, which tightens the binary case but leaves the physical assignment of those groups under-supported.

read the letter

The main takeaway is that this paper brings fresh multi-epoch high-resolution spectra of NaSt1 and reports radial velocity changes in 35 emission lines that fall into two groups sharing a 310-day period but moving in opposite phases. The light-curve period matches, which helps exclude a 620-day ellipsoidal signal and makes pulsations less likely. They also add mid-IR dust modeling with two components and IFU data showing the nebula expands at about 31 km/s for a dynamical age near 40 years. These are concrete new measurements for this object. The work is straightforward on the data side: they present the period fits, note the phase offset, and check consistency across wavelengths. That part holds up as useful observational progress on a proposed post-mass-transfer system. The softer spot is the step that ties one line group to the stripped primary's wind and the other to a wind-collision zone. The paper infers this mainly from the phase difference, but it does not include line-by-line identifications, profile modeling, or tests that would rule out other origins such as layered wind zones or unrelated variability. Without that, the opposing-phase signal is interesting but not yet a fully independent confirmation of a companion. Readers focused on massive binaries, stripped stars, or Galactic supernova progenitor candidates will get value from the new numbers and the multi-wavelength coverage. The analysis is honest about the data even if the interpretation of the lines could be tightened. I would bring this to a reading group on stellar evolution or binaries. I would not cite it in my own work in the next year. It deserves peer review because the RV dataset is new and directly testable.

Referee Report

2 major / 2 minor

Summary. The manuscript reports multi-epoch high-resolution optical spectroscopy (R ≃ 80,000) of NaSt1, identifying two groups of emission lines whose radial velocities vary with a shared period of 310 ± 6 d but opposite phases. These are interpreted as tracing the optically thick wind of a stripped primary and the wind-wind collision region with a companion, constituting evidence for binarity. Supporting observations include long-term multiband photometry (ruling out 620 d ellipsoidal modulation), 1–5 μm spectroscopy modeled with two optically thin dust components, and IFU spectroscopy resolving the nebula with ~31 km s⁻¹ expansion implying a ~40 yr dynamical age.

Significance. If the line-to-region mapping holds, the work supplies direct radial-velocity evidence for a post-mass-transfer massive binary and a Galactic analog to stripped-envelope supernova progenitors. The multi-epoch high-resolution spectroscopy yielding opposing-phase signals, combined with the light-curve period consistency that excludes the ellipsoidal alternative, represents a clear observational strength and a falsifiable test of the binary hypothesis.

major comments (2)

[RV analysis section] RV analysis section: The division of the emission lines into two groups and their specific association with the primary wind versus the wind-collision region rests solely on the shared 310 d period and phase opposition. No line identifications, profile modeling, or radiative-transfer verification is provided to exclude alternatives such as stratified wind zones or non-orbital variability; this mapping is load-bearing for the binarity claim.
[Line selection and measurement subsection] Line selection and measurement subsection: Details of how the 35 lines were chosen, the precise RV extraction method, and the per-line velocity uncertainties are not reported. These are required to evaluate the statistical significance of the period fit and the robustness of the opposing-phase detection.

minor comments (2)

[Abstract] Abstract: clarify whether 'two groups of 35 emission lines' refers to 35 lines total or 35 lines per group.
[Dust modeling paragraph] Dust modeling paragraph: state the specific assumptions (e.g., grain properties, geometry) and any fitting code or references used for the hot and warm components.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough review and for recognizing the significance of our radial velocity evidence for the binarity of NaSt1. We address each of the major comments below.

read point-by-point responses

Referee: [RV analysis section] The division of the emission lines into two groups and their specific association with the primary wind versus the wind-collision region rests solely on the shared 310 d period and phase opposition. No line identifications, profile modeling, or radiative-transfer verification is provided to exclude alternatives such as stratified wind zones or non-orbital variability; this mapping is load-bearing for the binarity claim.

Authors: The association of the two groups with the primary wind and the wind-wind collision region is indeed based on the observed RV period and phase opposition, which is difficult to explain without invoking orbital motion in a binary system. In the revised manuscript, we will add the specific identifications of the lines in each group and include a more detailed discussion of the line profiles to support the mapping. While a full radiative transfer calculation is beyond the scope of this paper, we will explicitly address why alternatives like stratified winds are unlikely given the clear phase opposition and the consistency with the photometric period. We believe this strengthens the binarity claim without overclaiming. revision: partial
Referee: [Line selection and measurement subsection] Details of how the 35 lines were chosen, the precise RV extraction method, and the per-line velocity uncertainties are not reported. These are required to evaluate the statistical significance of the period fit and the robustness of the opposing-phase detection.

Authors: We agree that these details are essential for assessing the robustness of our results. In the revised manuscript, we will expand the relevant subsection to describe the selection criteria for the 35 emission lines (focusing on unblended, high signal-to-noise lines), the method used for RV extraction (e.g., centroid fitting or Gaussian profile fitting), and provide the per-line velocity uncertainties. This will enable a better evaluation of the period significance and the opposing-phase detection. revision: yes

Circularity Check

0 steps flagged

No circularity: central binarity claim follows directly from period fits to new RV data.

full rationale

The paper measures radial velocities from 35 emission lines across multiple epochs, fits a common 310-day period with opposing phases, and compares it to the light-curve period. These steps are data-driven extractions and statistical fits with no equations that define the target period or binary geometry in terms of themselves. No self-citations, ansatzes, or uniqueness theorems are invoked to force the result. The physical association of line groups is an interpretation, not a definitional reduction. The derivation chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The interpretation rests on associating specific emission-line groups with physical wind components and on treating the fitted 310-day period as orbital; these steps introduce domain assumptions about line formation in massive-star winds rather than new free parameters or invented entities.

free parameters (2)

RV period = 310 ± 6 d
Fitted directly to the time series of emission-line velocities
Dust temperatures and masses = Th ≈ 1230 K, Mh ≈ 2×10^{-10} M⊙; Tc ≈ 660 K, Mc ≈ 3×10^{-8} M⊙
Obtained by fitting two optically thin dust components to the 1-5 μm spectrum

axioms (2)

domain assumption The two groups of emission lines trace the optically thick wind of the stripped primary and the wind-wind collision region
Invoked to interpret the opposing-phase RV curves as binary motion
domain assumption The observed RV period is the orbital period of the binary
Used to rule out pulsations and ellipsoidal modulation via phase comparison with the light curve

pith-pipeline@v0.9.0 · 5719 in / 1633 out tokens · 59486 ms · 2026-05-10T12:00:35.419795+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

51 extracted references · 48 canonical work pages · 2 internal anchors

[1]

P., Tollerud, E

Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068

work page doi:10.1051/0004-6361/201322068 2013
[2]

C., Kulkarni, S

Bellm, E. C., Kulkarni, S. R., Graham, M. J., et al. 2019, PASP, 131, 018002, doi: 10.1088/1538-3873/aaecbe

work page doi:10.1088/1538-3873/aaecbe 2019
[3]

P., & Mathews, W

Cox, D. P., & Mathews, W. G. 1969, ApJ, 155, 859, doi: 10.1086/149916

work page doi:10.1086/149916 1969
[4]

Crowther, P. A. 2007, ARA&A, 45, 177, doi: 10.1146/annurev.astro.45.051806.110615

work page doi:10.1146/annurev.astro.45.051806.110615 2007
[5]

, keywords =

Crowther, P. A., & Smith, L. J. 1999, Monthly Notices of the Royal Astronomical Society, 308, 82, doi: 10.1046/j.1365-8711.1999.02707.x

work page doi:10.1046/j.1365-8711.1999.02707.x 1999
[6]

C., Vacca, W

Cushing, M. C., Vacca, W. D., & Rayner, J. T. 2004, PASP, 116, 362, doi: 10.1086/382907

work page doi:10.1086/382907 2004
[7]

J., Kasliwal, M

De, K., Hankins, M. J., Kasliwal, M. M., et al. 2020a, Publications of the Astronomical Society of the Pacific, 132, 025001, doi: 10.1088/1538-3873/ab6069

work page doi:10.1088/1538-3873/ab6069
[8]

De, K., Ashley, M. C. B., Andreoni, I., et al. 2020b, The Astrophysical Journal Letters, 901, L7, doi: 10.3847/2041-8213/abb3c5 Djuraˇ sevi´ c, G., Vince, I., & Atanackovi´ c, O. 2008, The Astronomical Journal, 136, 767, doi: 10.1088/0004-6256/136/2/767

work page doi:10.3847/2041-8213/abb3c5 2041
[9]

T., & Lee, H

Draine, B. T., & Lee, H. M. 1984, ApJ, 285, 89, doi: 10.1086/162480

work page doi:10.1086/162480 1984
[10]

V., Li, W

Filippenko, A. V., Li, W. D., Treffers, R. R., & Modjaz, M. 2001, in Astronomical Society of the Pacific Conference

2001
[11]

Fitzpatrick, E. L. 1999, PASP, 111, 63, doi: 10.1086/316293

work page doi:10.1086/316293 1999
[12]

doi:10.1086/670067 , eprint =

Foreman-Mackey, D., Hogg, D. W., Lang, D., & Goodman, J. 2013, Publications of the Astronomical Society of the Pacific, 125, 306, doi: 10.1086/670067

work page doi:10.1086/670067 2013
[13]

D., Chevalier, R

Fox, O. D., Chevalier, R. A., Dwek, E., et al. 2010, The Astrophysical Journal, 725, 1768, doi: 10.1088/0004-637X/725/2/1768

work page doi:10.1088/0004-637x/725/2/1768 2010
[14]

Summary of the contents and survey properties

Gagne, M., Townsley, L., Corcoran, M., et al. 2010, in AAS/High Energy Astrophysics Division, Vol. 11, AAS/High Energy Astrophysics Division #11, 17.12 Gaia Collaboration, Brown, A. G. A., Vallenari, A., et al. 2021, A&A, 649, A1, doi: 10.1051/0004-6361/202039657

work page doi:10.1051/0004-6361/202039657 2010
[15]

A., Joyce, M., & Moln´ ar, L

Goldberg, J. A., Joyce, M., & Moln´ ar, L. 2024, The Astrophysical Journal, 977, 35, doi: 10.3847/1538-4357/ad87f4

work page doi:10.3847/1538-4357/ad87f4 2024
[16]

Harris, K

Harris, C. R., Millman, K. J., van der Walt, S. J., et al. 2020, Nature, 585, 357, doi: 10.1038/s41586-020-2649-2

work page doi:10.1038/s41586-020-2649-2 2020
[17]

N., Tonry, J

Heinze, A. N., Tonry, J. L., Denneau, L., et al. 2018, The Astronomical Journal, 156, 241, doi: 10.3847/1538-3881/aae47f

work page doi:10.3847/1538-3881/aae47f 2018
[18]

Hunter, J. D. 2007, Computing in Science & Engineering, 9, 90, doi: 10.1109/MCSE.2007.55

work page doi:10.1109/mcse.2007.55 2007
[19]

S., Babler, B

Indebetouw, R., Mathis, J. S., Babler, B. L., et al. 2005, ApJ, 619, 931, doi: 10.1086/426679

work page doi:10.1086/426679 2005
[20]

Z., Kochanek, C

Jayasinghe, T., Stanek, K. Z., Kochanek, C. S., et al. 2020, Monthly Notices of the Royal Astronomical Society, 493, 4186, doi: 10.1093/mnras/staa499

work page doi:10.1093/mnras/staa499 2020
[21]

, keywords =

Kochanek, C. S., Shappee, B. J., Stanek, K. Z., et al. 2017, Publications of the Astronomical Society of the Pacific, 129, 104502, doi: 10.1088/1538-3873/aa80d9

work page doi:10.1088/1538-3873/aa80d9 2017
[22]

Laor, A., & Draine, B. T. 1993, ApJ, 402, 441, doi: 10.1086/172149 Radial velocity evidence for NaSt115 0.75 1.00 1.25 1.50 1.75 2.00 2.25 Continuum Normalized Flux He I λ3889 1.0 1.5 2.0 2.5 3.0 3.5 [Fe III] λ4658 2 4 6 8 He II λ4686 0.8 1.0 1.2 1.4 1.6 1.8 2.0 [Fe III] λ4701 1.0 1.5 2.0 2.5 3.0 He I λ4713 1.0 1.2 1.4 1.6 1.8 2.0 2.2 2.4 He II λ4859 1 2 ...

work page doi:10.1086/172149 1993
[23]

M., Tinyanont, S., Hankins, M

Lau, R. M., Tinyanont, S., Hankins, M. J., et al. 2021, The Astrophysical Journal, 922, 5, doi: 10.3847/1538-4357/ac2237

work page doi:10.3847/1538-4357/ac2237 2021
[24]

1990, ApJ, 362, 267, doi: 10.1086/169263

Luo, D., McCray, R., & Mac Low, M.-M. 1990, ApJ, 362, 267, doi: 10.1086/169263

work page doi:10.1086/169263 1990
[25]

The Zwicky Transient Facility: Data Processing, Products, and Archive

Masci, F. J., Laher, R. R., Rusholme, B., et al. 2018, Publications of the Astronomical Society of the Pacific, 131, 018003, doi: 10.1088/1538-3873/aae8ac

work page internal anchor Pith review doi:10.1088/1538-3873/aae8ac 2018
[26]

D., et al

Mauerhan, J., Smith, N., Van Dyk, S. D., et al. 2015, MNRAS, 450, 2551, doi: 10.1093/mnras/stv257 16W angnok et al. A=4.12+0.08 °0.07 0.930 0.945 0.960 0.975 ! !=0.95+0.01 °0.01 ° 20 .1 ° 19 .8 ° 19 .5 ° 19 .2 ¡ ¡=°19.65+0.14 °0.14 3.90 4.05 4.20 4.35 A ° 2.70 ° 2.55 ° 2.40 ° 2.25 C 0.930 0.945 0.960 0.975 ! ° 20 .1 ° 19 .8 ° 19 .5 ° 19 .2 ¡ ° 2.70 ° 2.55...

work page doi:10.1093/mnras/stv257 2015
[27]

Medina, S. N. X., Urquhart, J. S., Dzib, S. A., et al. 2019, A&A, 627, A175, doi: 10.1051/0004-6361/201935249

work page doi:10.1051/0004-6361/201935249 2019
[28]

C., et al

Morrissey, P., Matuszewski, M., Martin, D. C., et al. 2018, ApJ, 864, 93, doi: 10.3847/1538-4357/aad597

work page doi:10.3847/1538-4357/aad597 2018
[29]

Morton, D. C. 1991, ApJS, 77, 119, doi: 10.1086/191601

work page doi:10.1086/191601 1991
[30]

J., Stephenson, C., & MacConnell, D

Nassau, J. J., Stephenson, C., & MacConnell, D. 1965, Luminous Stars in the Northern Milky Way...: VI. (Hamburger sternwarte Warner and Swasey observatory)

1965
[31]

2023, KCWI DRP: Keck Cosmic Web Imager Data Reduction Pipeline in Python,, Astrophysics Source Code Library, record ascl:2301.019 http://ascl.net/2301.019

Rizzi, L. 2023, KCWI DRP: Keck Cosmic Web Imager Data Reduction Pipeline in Python,, Astrophysics Source Code Library, record ascl:2301.019 http://ascl.net/2301.019

2023
[32]

T., & Vogt, S

Lockwood, C. T., & Vogt, S. S. 2010, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 7735, Ground-based and Airborne Instrumentation for Astronomy III, ed. I. S. McLean, S. K. Ramsay, & H. Takami, 77354K, doi: 10.1117/12.857726

work page doi:10.1117/12.857726 2010
[33]

T., Toomey, D

Rayner, J. T., Toomey, D. W., Onaka, P. M., et al. 2003, PASP, 115, 362, doi: 10.1086/367745

work page doi:10.1086/367745 2003
[34]

doi:10.1126/science.1223344 , eprint =

Sana, H., de Mink, S. E., de Koter, A., et al. 2012, Science, 337, 444, doi: 10.1126/science.1223344

work page doi:10.1126/science.1223344 2012
[35]

2022, A&A, 668, A57, doi: 10.1051/0004-6361/202244391

Sarangi, A. 2022, A&A, 668, A57, doi: 10.1051/0004-6361/202244391

work page doi:10.1051/0004-6361/202244391 2022
[36]

2023, Monthly Notices of the Royal Astronomical Society, 523, 6048, doi: 10.1093/mnras/stad1681

Shahbandeh, M., Sarangi, A., Temim, T., et al. 2023, Monthly Notices of the Royal Astronomical Society, 523, 6048, doi: 10.1093/mnras/stad1681

work page doi:10.1093/mnras/stad1681 2023
[37]

, keywords =

Shappee, B. J., Prieto, J. L., Grupe, D., et al. 2014, The Astrophysical Journal, 788, 48, doi: 10.1088/0004-637X/788/1/48

work page doi:10.1088/0004-637x/788/1/48 2014
[38]

Sokal, K. R. 2010, The Astronomical Journal, 139, 825, doi: 10.1088/0004-6256/139/3/825

work page doi:10.1088/0004-6256/139/3/825 2010
[39]

F., Cutri , R

Skrutskie, M. F., Cutri, R. M., Stiening, R., et al. 2006, AJ, 131, 1163, doi: 10.1086/498708

work page doi:10.1086/498708 2006
[40]

Smith, J. D. T., & Houck, J. R. 2001, AJ, 121, 2115, doi: 10.1086/319968

work page doi:10.1086/319968 2001
[41]

doi:10.1046/j.1365-8711.2002.05889.x , archiveprefix =

Smith, N. 2002, MNRAS, 337, 1252, doi: 10.1046/j.1365-8711.2002.05966.x

work page doi:10.1046/j.1365-8711.2002.05966.x 2002
[42]

2014, ARA&A, 52, 487, doi: 10.1146/annurev-astro-081913-040025

Smith, N. 2014, ARA&A, 52, 487, doi: 10.1146/annurev-astro-081913-040025

work page doi:10.1146/annurev-astro-081913-040025 2014
[43]

2011, MNRAS, 415, 2101, doi: 10.1111/j.1365-2966.2011.18820.x

Smith, N., Gehrz, R. D., Campbell, R., et al. 2011, MNRAS, 418, 1959, doi: 10.1111/j.1365-2966.2011.19614.x

work page doi:10.1111/j.1365-2966.2011.19614.x 2011
[44]

D., Stahl, O., Balick, B., & Kaufer, A

Smith, N., Gehrz, R. D., Stahl, O., Balick, B., & Kaufer, A. 2002, The Astrophysical Journal, 578, 464, doi: 10.1086/342365 Radial velocity evidence for NaSt117

work page doi:10.1086/342365 2002
[45]

2020, Monthly Notices of the Royal Astronomical Society, 492, 5897, doi: 10.1093/mnras/staa061 The Astropy Collaboration, Price-Whelan, A

Smith, N., E Andrews, J., Moe, M., et al. 2020, Monthly Notices of the Royal Astronomical Society, 492, 5897, doi: 10.1093/mnras/staa061 The Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, The Astronomical Journal, 156, 123, doi: 10.3847/1538-3881/aabc4f

work page doi:10.1093/mnras/staa061 2020
[46]

D., Shahbandeh, M., et al

Tinyanont, S., Fox, O. D., Shahbandeh, M., et al. 2025, The Astrophysical Journal, 985, 198, doi: 10.3847/1538-4357/adccc0

work page doi:10.3847/1538-4357/adccc0 2025
[47]

ATLAS: A High-Cadence All-Sky Survey System

Tonry, J. L., Denneau, L., Heinze, A. N., et al. 2018, Publications of the Astronomical Society of the Pacific, 130, 064505, doi: 10.1088/1538-3873/aabadf

work page internal anchor Pith review doi:10.1088/1538-3873/aabadf 2018
[48]

Usov, V. V. 1992, ApJ, 389, 635, doi: 10.1086/171236

work page doi:10.1086/171236 1992
[49]

D., Cushing, M

Vacca, W. D., Cushing, M. C., & Rayner, J. T. 2003, PASP, 115, 389, doi: 10.1086/346193

work page doi:10.1086/346193 2003
[50]

, keywords =

Vogt, S. S., Radovan, M., Kibrick, R., et al. 2014, PASP, 126, 359, doi: 10.1086/676120

work page doi:10.1086/676120 2014
[51]

E., & Barlow, M

Wright, A. E., & Barlow, M. J. 1975, Monthly Notices of the Royal Astronomical Society, 170, 41, doi: 10.1093/mnras/170.1.41

work page doi:10.1093/mnras/170.1.41 1975