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V4141 Sgr: Outflows and repeated outbursts

T0 review · 2 major / 7 minor · reviewed 2026-08-16 · deepseek-v4-flash

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Pith's one-line read V4141 Sgr, a symbiotic binary in Sagittarius, is undergoing a new optical outburst that began around September 2024, with spectra showing high-velocity, optically thick outflows and a possible bipolar jet; combined with plate records, the…

desk verdict A solid observational letter that catches V4141 Sgr in a fresh outburst with real P Cygni outflows; the 1940s historical brightening is plausible but needs a quantitative DASCH error check. read the letter →

arxiv 2504.16806 v1 pith:NFF5M2ON submitted 2025-04-23 astro-ph.SR

Jaroslav Merc , Joanna Miko{l}ajewska , Thomas Petit , Berto Monard , Stéphane Charbonnel , Olivier Garde , Pascal Le Dû , Lionel Mulato
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Tadashi Kojima
This is my paper · ORCID
classification astro-ph.SR
keywords symbioticstarsV4141SgrPCygniprofilesstellaroutflowsbipolarjetsslownovaelong-termphotometryphotographicplates
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The pith

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

The reading

This paper establishes that V4141 Sgr, a poorly studied symbiotic star, is a repeating outburst system. The ongoing brightening, first noticed in February 2025, began around September 2024 and is still rising; spectra show P Cygni profiles with blue-shifted absorption at 1000–1500 km/s, meaning the outburst is ejecting optically thick material, with a redshifted H-alpha component that may trace a bipolar jet. Combining century-long photographic records with modern surveys, the authors show the star also brightened in the 1940s and from the 1960s/1970s until 1990. If correct, V4141 Sgr joins a small group of symbiotic stars with detected outflows and repeated outbursts, and its current event differs from classical symbiotic eruptions in that the hot component's luminosity rises sharply.

What carries the argument

The argument rests on two observational pillars. The first is the P Cygni profile, a spectral signature in which a strong emission line is overlaid by blue-shifted absorption; here it appears in Balmer lines at 1000–1500 km/s and acts as the direct evidence for an optically thick, high-velocity outflow. The second is the century-long photometric light curve built from DASCH photographic plates, Kondrat'eva's V-band measurements, and ASAS-SN/ATLAS/Gaia survey data, which lets the authors identify separate outburst episodes and bound the quiescent intervals between them. The comparison of V4141 Sgr with neighboring field stars on individual plates is what supports the reality of the 1940s brightening.

What would settle it

Re-reduce the DASCH plates epoch-by-epoch with a per-plate zero-point derived from the three comparison stars shown in Fig. 4; if the 1944–1949 brightening disappears or drops below the scatter of the neighbor-star differences, the claim of a 1940s outburst collapses. Separately, a high-resolution spectrum taken during the current outburst would settle whether the redshifted H-alpha component is a true jet: a jet should show a distinct, Doppler-shifted satellite feature rather than a broad line wing.

Watch

Extended reading notes

Core claim

The central claim is that V4141 Sgr is a symbiotic star caught in a recurring cycle of outbursts, with at least three brightenings over the last century. The 2024/2025 event is marked by P Cygni profiles — emission lines with broad blue-shifted absorption — at velocities of about 1000 to 1500 km/s, indicating a dense, optically thick wind; an extra redshifted component on H-alpha suggests a collimated outflow or jet. The long-term light curve, assembled from Harvard plate data and modern surveys, reveals a brightening in the 1940s and a long event from the 1960s/1970s to 1990 whose spectral evolution resembled slow symbiotic novae such as RR Tel and AG Peg. The paper therefore places V4141 Sgr among the few symbiotic stars where optical spectra show outflows and possible jets, and argues that its history of repeated eruptions makes it a prime target for continued monitoring.

Load-bearing premise

The repeated-outburst story hinges on the 1940s brightening seen in Harvard plate data being a real change of the star rather than a calibration or plate-to-plate artifact; the data are sparse and the zero-point uncertainty is not quantified.

Editorial extensions

If this is right

  • If the current outburst continues to rise, follow-up spectroscopy over the coming months should reveal whether the jet component strengthens and whether the P Cygni absorption persists.
  • The three separated outbursts imply recurrence timescales of roughly 15–35 years, so V4141 Sgr can be added to the small group of symbiotic stars with documented repeated eruptions.
  • The luminosity increase of the hot component to about 5000 solar luminosities during the 2025 event (a lower limit) distinguishes this outburst from constant-luminosity classical symbiotic eruptions and aligns it with systems like AG Dra and Gaia18aen.
  • The 790-day low-amplitude variability seen in quiescent ATLAS and Gaia data, if orbital, would make V4141 Sgr one of the few symbiotic stars with a measured period before its outburst.
  • The detection of P Cygni profiles and a possible jet means V4141 Sgr can serve as a test bed for models of optically thick winds and jet launching in symbiotic binaries.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • If the 1940s brightening is real, the recurrence pattern (roughly 1940s, 1970s, 2020s) suggests an underlying clock or a common trigger; one testable extension is to search the DASCH plates for fainter precursor events around 1910–1930, which the paper's sparse data cannot rule out.
  • The possible bipolar jet could be confirmed with higher-resolution spectroscopy: if the redshifted H-alpha component persists and shows velocity structure, V4141 Sgr would join Z And and BF Cyg in having resolved jet kinematics.
  • The paper's inference that the hot component luminosity rises by a factor of several during outburst, if confirmed by future UV/X-ray observations, would imply a thermonuclear trigger rather than a pure accretion-disk instability, linking V4141 Sgr to slow symbiotic novae rather than classical Z And-type eruptions.
  • A direct extension is to re-reduce the DASCH plates with per-plate calibration using the three comparison stars to check whether the 1940s brightening's slow decline is consistent across independent plate series.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

2 major / 7 minor

Summary. This paper reports the discovery and characterization of an ongoing outburst of the symbiotic star V4141 Sgr. The authors present low-resolution optical spectra from February and March 2025 showing P Cygni profiles in the Balmer lines with blue-shifted absorption at about -1000 to -1500 km/s, and an additional redshifted H-alpha emission component, indicating an optically thick outflow and possibly jets. Photometry from the authors, ASAS-SN, ATLAS, and Gaia shows a brightening beginning around September 2024, with amplitude 2.6-3.5 mag depending on band and a blueing of the color. Combining historical DASCH plates and literature magnitudes, they construct a >100-year light curve and claim at least three outburst states: a 1940s brightening, a prolonged 1960s/70s-1990 event resembling a slow symbiotic nova, and the current one. They also derive hot-component temperatures and luminosities at several epochs and argue that the current outburst is luminosity-driven. The paper concludes that V4141 Sgr is a rare recurring symbiotic system with detected outflows.

Significance. If the claims hold, V4141 Sgr would be a valuable target for studying recurrent symbiotic outbursts and outflows/jets in symbiotic stars. The strength of the paper lies in the direct presentation of spectroscopic features (Fig. 2) and multi-survey photometry, and in the use of archival plates with comparison stars. The historical recurrence claim, however, rests on the reality of the 1940s brightening, which is currently supported only by visual plate inspection and sparse photometry without an error budget. The paper makes falsifiable predictions (continued brightening, further spectral evolution) and is generally well-connected to the literature. The central result is promising, but the quantitative case for the 1940s event needs strengthening to support the 'repeated outbursts' framing.

major comments (2)
  1. [3.2, Fig. 4] The 1940s brightening is a load-bearing element of the abstract's 'multiple outbursts' claim and of Section 4.2's uniqueness statement, yet its reality is asserted as 'undoubtedly' based only on a visual comparison with three field stars on a small number of DASCH plates. No differential photometry, per-plate zero-point uncertainties, or variability check of the comparison stars is provided. Given that DASCH photometry is known to have plate-to-plate systematics at the level of a few tenths of a magnitude, comparable to the contrast between the claimed bright and faint states, the authors should either present a quantitative reduction of these plates or soften the claim and explicitly state that the 1940s event is probable but unconfirmed.
  2. [3.2, Fig. 3] The long-term light curve in Fig. 3 combines photographic B-band data with V-band magnitudes from literature without applying filter shifts or plotting error bars. As a result, the significance of the 1940s brightening relative to the quiescent level cannot be independently assessed. The authors should include per-epoch uncertainties and a description of the zero-point calibration (e.g., scatter around APASS B standards) so that the amplitude of the historical events can be judged against the noise.
minor comments (7)
  1. [3.1] The word 'qiescent' in the sentence 'reported in the qiescent spectra' should be 'quiescent'.
  2. [3.1] The sentence 'The data confirms that the star appears significantly bluer' should use 'confirm' to agree with the plural subject 'data'.
  3. [3.1, Fig. 2] The claimed redshifted H-alpha jet component is not quantified; a velocity or profile decomposition would help the reader evaluate the jet interpretation.
  4. [4.2] The phrase 'This is not the first instance where a later eruption' would read better as 'in which'.
  5. [Appendix C] The assumption m_bol ≈ V_hot used to derive L_h ≈ 5000 L_sun should be justified, since a bolometric correction is expected for a hot component.
  6. [3.3] The statement that the ~790-day variation 'could be due to orbital motion' is appropriately hedged, but the paper does not give the amplitude of this variation; a brief quantitative value would be useful.
  7. [1] The sentence 'The object has since been included as such also in later symbiotic catalogs' is awkward; consider rewriting for clarity.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the outburst analysis is self-contained and the hot-component estimates rely on an independent published method.

full rationale

The paper does not derive results from its own inputs by construction. The recent outburst is inferred from fresh photometry and spectroscopy; the P Cygni profiles and brightness estimates are direct observations. The 1940s and 1970s outbursts are historical light-curve interpretations, not predictions folded into the analysis. The hot-component temperature and luminosity estimates in Appendix C use the published line-flux method of Mikolajewska et al. (1997) with explicit blackbody and case B assumptions, and they use line fluxes from independent archival spectra, so the derived values are not equivalent to an input fit. The symbiotic classification is supported by multiple independent diagnostics (Gaia BP/RP TiO bands, [O III] ratios, 2MASS colors) rather than resting solely on a self-citation. The weakest quantitative step, the 1940s DASCH brightening, is a possible calibration/systematics concern about sparse historical plates; it is an observational uncertainty, not a circularity in which the claim is assumed by its own definition. No equation or parameter is renamed as a prediction, and no uniqueness theorem from the same authors is invoked to force the choice. Overall circularity score: 0.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

The central claims rest on no new invented entities and no circularly fitted inputs. The ledger lists the adopted physical inputs (reddening, distance), the fitted quiescent periodicity, and the domain assumptions under which the historical plates, line fluxes, and quiescent spectra are interpreted. The possible bipolar jets are an inference from a known spectral feature, hedged by the authors as 'possibly' and 'likely', not a new entity introduced to explain the data.

free parameters (3)
  • Quiescent photometric periodicity = approximately 790 days
    Fitted to quiescent ATLAS and Gaia DR3 light curves that show significant scatter; no period uncertainty or significance is reported and the paper calls the variation 'seemingly sinusoidal'. It is a side result, not an input to the outburst claims.
  • Interstellar reddening E(B-V) = 1.2 mag (alternative 1.12 mag from Luna & Costa 2005)
    Adopted from Mikolajewska et al. (1997) for the hot-component luminosity estimates in Appendix C; the derived temperatures and luminosities scale directly with this value.
  • Distance to V4141 Sgr = 7 kpc
    Adopted from Mikolajewska et al. (1997), cited as roughly consistent with the Bailer-Jones et al. (2021) geometric (about 7.4 kpc) and photogeometric (about 6.0 kpc) distances; it normalizes the luminosities in Appendix C.
assumptions (4)
  • domain assumption DASCH photographic plate magnitudes, calibrated to APASS B, preserve genuine brightness differences across epochs for V4141 Sgr and its neighbor stars.
    The 1940s outburst claim rests on this calibration across heterogeneous plate series (Section 3.2, Fig. 4). Only relative brightness checks against three neighbors are given, with no per-plate zero-point error budget.
  • domain assumption Hot-component temperatures and luminosities can be recovered from He ii, He i, and H-beta line fluxes assuming a blackbody continuum and case B recombination.
    Appendix C applies this published method (Mikolajewska et al. 1997) and states the assumptions; the resulting values (35 to 55 kK in 1984, about 90 kK in 1987 and 2002, roughly 5000 Lsun in 2025 as a lower limit) carry those model assumptions.
  • domain assumption The quiescent state is represented reliably by the Gaia BP/RP mean spectrum (2014 to 2017), the 2MASS colors (2000), and the 1996 K-band spectrum.
    These datasets, separated by up to two decades, are treated as sampling the same quiescent S-type system; the classification and the 790 day variability discussion both depend on that equivalence.
  • domain assumption The 1960s/1970s to 1990 brightening was a slow-nova-like outburst as characterized in the cited literature.
    The abstract's claim that at least one outburst has 'characteristics typical of slow symbiotic novae' inherits the spectroscopic description from Kondrat'eva (2001) and Kondrat'eva et al. (2025); the paper does not re-derive that classification from the archival spectra.

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Pith. "Pith review of V4141 Sgr: Outflows and repeated outbursts." pith.science (2026). https://pith.science/paper/NFF5M2ON

@misc{pith2026250416806,
  author       = {Pith},
  title        = {Pith review of: V4141 Sgr: Outflows and repeated outbursts},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NFF5M2ON}},
  note         = {Machine review of arXiv:2504.16806}
}
read the original abstract

In this work, we analyze the ongoing brightening of the poorly studied symbiotic star V4141 Sgr and examine its long-term variability. We present new low-resolution spectroscopic observations of the system in its bright state and combine them with multi-color photometric data from our observations, ASAS-SN, ATLAS, and Gaia DR3. To investigate its long-term evolution, we also incorporate historical data, including photographic plates, constructing a light curve spanning more than a century. Our analysis reveals that V4141 Sgr has undergone multiple outbursts, with at least one exhibiting characteristics typical of "slow" symbiotic novae. The current outburst is characterized by the ejection of optically thick material and possibly bipolar jets, a phenomenon observed in only a small fraction of symbiotic stars. These findings establish V4141 Sgr as an intriguing target for continued monitoring.

Figures

Figures reproduced from arXiv: 2504.16806 by the authors.

Figure 1
Figure 1. Recent light curves of V4141 Sgr. A: Our photometric observa￾tions, together with data from ASAS-SN, ATLAS, and Gaia, covering the period from ∼2010 to 2025. The dashed sinusoidal curve represents the apparent long-term variability of the star. B: Zoomed-in view of the photometric evolution during the recent brightening. C: Color evolution derived from ATLAS c- and o-band observations. began as early as September 20… view at source ↗
Figure 4
Figure 4. DASCH photographic plates of V4141 Sgr at different epochs. The field of view is 120′′× 120′′. The position of V4141 Sgr is marked in the first image, along with three additional stars discussed in the text: (a) 2MASS J17502296-1953309, (b) 2MASS J17503040-1954169, and (c) 2MASS J17501606-1952414. DASCH plates. Due to the sparsity of data, it is not possible to precisely determine when this outburst began or when th… view at source ↗
Figure 3
Figure 3. Long-term photometry of V4141 Sgr. Older data include DASCH observations (calibrated to the B band), V magnitudes from Kondrat’eva (2001), including their assessment of the Palomar Survey value and from Kondrat’eva et al. (2025), and B magnitudes from the USNO-A2.0 catalog. The recent evolution is shown using our V data and ATLAS o-band observations, which have been shifted by +1.85 mag for clarity. For better reada… view at source ↗
Figures from the paper (1 more)
Figure 5
Figure 5. Figure 5: Gaia BP/RP spectrum of V4141 Sgr. The gray curve shows the flux multiplied by a factor of five to enhance the visibility of fainter features. Flux uncertainties, as reported in the Gaia DR3 catalog, are shown as shaded regions. The most prominent emission and absorptio…

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