Pith. sign in

REVIEW 4 major objections 6 minor 174 references

This paper claims that the first symbiotic super-soft X-ray source in the Magellanic Bridge, eRASSU J043115.8-711730, is powered by pulsation-boosted accretion onto a white dwarf rather than by orbital motion.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · deepseek-v4-flash

2026-08-01 02:25 UTC pith:SU6VZ4H3

load-bearing objection A genuine new symbiotic SSS in the Bridge, with a solid identification and a load-bearing pulsation claim that needs stronger evidence. the 4 major comments →

arxiv 2607.27730 v1 pith:SU6VZ4H3 submitted 2026-07-30 astro-ph.HE

eRASSU J043115.8-711730: The first pulsating symbiotic super-soft X-ray source in the Magellanic Bridge

Tathagata Saha , Chandreyee Maitra , Philip Charles , Frank Haberl , David Kaltenbrunner , Andrej Udalski , David Buckley , Itumenleng Monageng
show 4 more authors
Lee Townsend Manami Sasaki Sara Saeedi Mara Salvato
This is my paper
classification astro-ph.HE
keywords symbiotic binarysuper-soft X-ray sourceMagellanic Bridgered giant pulsationRoche-lobe overflowwhite dwarf accretionlong-period variabilityX-ray variability
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper argues that the deeply variable X-ray source eRASSU J043115.8-711730 in the Magellanic Bridge is a symbiotic binary: a white dwarf steadily burning accreted hydrogen, fed by a red-giant companion. Optical and infrared monitoring reveal a ~524-day cycle in which the giant brightens, reddens, and simultaneously the X-ray and UV emission intensify. The authors interpret the 'redder-when-brighter' trend as evidence that the giant is pulsating, not being irradiated by the white dwarf, and that the pulsation periodically drives Roche-lobe overflow, boosting the accretion rate to near-Eddington levels. If this reading is correct, J0431-71 is the first symbiotic source found in the Bridge, offering a rare window into the old stellar population of the tidal stream between the Magellanic Clouds.

Core claim

J0431–71 shows a single-temperature soft X-ray spectrum at kT~20–30 eV that switches on and off between surveys, reaching 3.2×10^37 erg/s in the 0.15–1 keV band when bright; a red-giant photosphere at ~3600 K; optical emission lines including Balmer, He II, Bowen fluorescence, [Fe X], and Raman-scattered O VI; and a 500–560-day periodicity that is in phase across optical, IR, UV, and X-ray bands. The mid-infrared color becomes redder as the source brightens, which the authors use to reject irradiation and identify the long-period modulation as stellar pulsation of the donor. They propose that during pulsation maximum the expanded red giant overflows its Roche lobe, raising the accretion rate

What carries the argument

The load-bearing mechanism is the ~524-day red-giant pulsation (a long-period variable): as the star's radius oscillates, it periodically fills its Roche lobe and dumps matter onto the white dwarf. The supporting diagnostic is the mid-infrared redder-when-brighter color trend, which distinguishes a cooler, larger, brighter photosphere (pulsation) from a heated, bluer one (irradiation). A slim accretion disk with high viscosity and the matching viscous timescale (430–634 days) is invoked to convert the pulsed mass transfer into the observed X-ray modulation.

Load-bearing premise

The classification of J0431–71 as a pulsating symbiotic source rests on the inference that its ~524-day modulation is the donor star's pulsation rather than orbital motion, an inference based on a sparse mid-infrared color trend covering only about three cycles with no radial-velocity or multi-mode pulsation confirmation.

What would settle it

A radial-velocity series that shows a Keplerian orbital period at 524 days (or any period) with a semi-amplitude typical of a giant in a binary, while the photometric period shows no corresponding orbital phase coherence, or vice versa; alternatively, high-cadence photometry that resolves multiple pulsation periods (e.g., period ratios) would confirm the long-period-variable interpretation, while a single strict period with no harmonics would favor orbit. A direct measurement of the photospheric temperature that rises during the bright phase would falsify the redder-when-brighter pulsation cla

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • J0431–71 becomes the first symbiotic binary discovered in the Magellanic Bridge, demonstrating that X-ray surveys can uncover compact-object-accreting systems among the Bridge's old stars.
  • The pulsation-driven Roche-lobe overflow mechanism offers a general explanation for long-period symbiotic super-soft sources that vary in phase in the optical and X-ray.
  • The system's bright state is predictable from the donor's ~524-day pulsation phase, allowing targeted X-ray and UV observations at maximum accretion.
  • The large inferred accretion rate and near-Eddington luminosity imply a massive white dwarf (>0.6 solar masses), relevant for Type Ia supernova progenitors in low-metallicity environments.
  • Kinematics and position place the source in the LMC-periphery/Bridge drift population, linking it to the tidal interaction history of the Magellanic Clouds.

Where Pith is reading between the lines

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

  • The pulsation-vs-orbit question is directly testable: a radial-velocity curve that shows a Keplerian orbital period different from the photometric 524-day period (or none at that period) would confirm pulsation; a matching orbital signature would overturn the interpretation.
  • If pulsation-driven Roche-lobe overflow is correct, similar symbiotic super-soft sources in the LMC/SMC with long-period variability should show the same redder-when-brighter signature and in-phase X-ray brightening, whereas irradiation-dominated systems should appear bluer when brighter.
  • The assumed 50 kpc distance scales all luminosities and accretion rates, but the pulsation-vs-orbit argument depends only on morphology and phase alignment, not on distance.
  • The presence of Raman-scattered O VI lines suggests a strong far-UV ionizing continuum; future UV spectroscopy could test whether the UV component arises from the nebula rather than from the white dwarf's Rayleigh-Jeans tail.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 6 minor

Summary. The paper reports multi-wavelength observations of eRASSU J043115.8-711730, an eROSITA-discovered super-soft X-ray source in the Magellanic Bridge region. Using XMM-Newton, eROSITA, Swift, SALT, OGLE, ATLAS, ASAS-SN, WISE, and Gaia data, the authors classify the source as an α-type symbiotic SSS with a red-giant companion. They identify a ~524-day optical/IR periodicity, in-phase X-ray/UV variability, a redder-when-brighter WISE W1−W2 trend, and optical emission lines including [Fe X] and Raman-scattered O VI. They interpret the periodicity as a donor-star pulsation that drives variable Roche-lobe overflow accretion onto a white dwarf, with mass-transfer rates up to ~1.7e-6 Msun/yr, and claim this makes J0431-71 the first symbiotic source discovered in the Magellanic Bridge.

Significance. If the central interpretation holds, the source would be the first symbiotic SSS in the Magellanic Bridge and a rare example of pulsation-driven mass transfer in a symbiotic system. The paper usefully assembles a rich multi-epoch dataset and applies appropriate Bayesian spectral fitting, and the qualitative classification as an α-type symbiotic SSS with a red-giant donor is reasonably supported. However, the pulsation-versus-orbital distinction is not yet secured, and the Magellanic Bridge membership is not conclusively established. The paper's value is more in the multiwavelength characterization than in the currently load-bearing pulsation interpretation.

major comments (4)
  1. [§5, Fig. 4e, §8.3] The 'redder-when-brighter' WISE W1−W2 trend is the primary evidence against irradiation and for a pulsating donor. However, for a ~3600 K blackbody, W1 (3.4 μm) and W2 (4.6 μm) lie on the Rayleigh-Jeans tail, where the W1−W2 color is nearly temperature-independent to first order. The observed color change therefore cannot be directly interpreted as 'lower effective temperature during bright phases' without a detailed model of the donor's spectral energy distribution (e.g., molecular opacities, circumstellar material). The trend is also based on only a handful of WISE epochs (~2 per 524-d cycle, with a ~540-d peak spacing), so aliasing and contamination from HD 270522 (30″ away) need quantitative assessment before this can support the pulsation scenario.
  2. [§8.3] The exclusion of an orbital origin for the 524-d period rests on tidal circularization arguments and the color trend, but no radial-velocity curve is presented. A low-eccentricity or high-inclination orbit could produce the ~0.4 mag optical modulation and phase-locked X-ray/UV variability. The X-ray/UV phase alignment is based on only four positive X-ray detections and two upper limits; with this sampling, phase offsets of ~0.2 in period are not excluded. The conclusion that 'these observations ... impose the requirement of a stellar-pulsation-enhanced variable accretion' is therefore stronger than the data allow.
  3. [§8.6, Abstract] The abstract and title describe J0431-71 as the first symbiotic source in the Magellanic Bridge, but §8.6 states that the position and proper motion are equally consistent with LMC membership, an SMC accreted population, or Bridge drift. Since the kinematic evidence does not uniquely place the system in the Bridge, the 'first in the Bridge' claim is not supported by the analysis presented.
  4. [Appendix D, §8.3] The viscous-timescale consistency check is not independent: M_WD=1.0 M_sun, α=0.5, and H/R=0.5 are adopted (not measured) so that t_visc spans 430–634 d and brackets the observed 524-d period. This is a posteriori parameter tuning rather than a test of the pulsation-driven RLOF scenario. It should be presented as such, and the sensitivity of the conclusion to these choices should be discussed.
minor comments (6)
  1. [Table 1] eRASS2 and eRASS3 are both listed with observation date 2021-01-15; given the text states detections in the second and third all-sky scans, these dates should be corrected (likely eRASS2 in 2020 and eRASS3 in 2021).
  2. [§3.3] The 2026 Swift observation is described as taken, but the manuscript is a 2026 preprint; if the data were obtained in 2026, the exact date should be specified in Table 1.
  3. [Appendix E, Eq. E1] The expression for β_OX uses 'BP+RP/5'; parentheses should clarify whether it is (BP+RP)/5.
  4. [Fig. 4e] The red-dashed line for the SALT epoch is difficult to distinguish in the figure; consider a different line style or annotation.
  5. [§5, Table 3] The peak periods across bands span 501–557 d with FWHMs of 43–200 d; the paper should quantify whether these are statistically consistent with a single period rather than qualitatively stating they are consistent.
  6. [§8.2] The bolometric correction BC_I is assumed from a 3600 K blackbody; the sensitivity of L_bol and the inferred stellar radius to this assumption is not discussed.

Circularity Check

0 steps flagged

No significant circularity: the classification rests on independent observables; Appendix D is a post-hoc consistency check, not a fitted prediction.

full rationale

J0431-71's characterization is assembled from independent observables: the eRASS/XMM spectra give a kT≈20–30 eV super-soft component; the SALT spectrum gives Balmer, He II, [Fe X], Bowen, and Raman O VI lines; the Gaia CMD and infrared CMD place the companion on the red-giant branch; OGLE/ATLAS/ASAS-SN periodograms give 500–560 d periodicities; WISE W1−W2 shows a quasi-periodic redder-when-brighter trend. None of these inputs is defined in terms of the 'pulsating symbiotic' conclusion. The §8.3 pulsation argument is an interpretation of the observed color trend and phase relations, not a relation that holds by construction. Appendix D computes t_visc from a standard alpha-disk/slim-disk formula with adopted parameters (M_WD=1.0 Msun, alpha=0.5, H/R=0.5, donor mass 1–5 Msun); while the chosen values do bracket the 524 d period, the formula does not contain the observed period as an input and no parameter is fitted to that period, so the agreement is a consistency check rather than a constructed prediction. The paper also explicitly concedes in §8.3 that it cannot directly constrain the total mass because it assumes the periodicity is pulsational—a genuine evidentiary limitation relevant to correctness, but not circularity. Self-citations (Haberl et al. 2023; Yang et al. 2026; Maitra & Haberl 2022; Schneider et al. 2022; Maitra et al. in prep) are contextual and none carries a load-bearing uniqueness theorem or an unverified ansatz on which the central claim depends. The central derivation is therefore self-contained with respect to its observables, and the circularity score is low.

Axiom & Free-Parameter Ledger

10 free parameters · 7 axioms · 0 invented entities

The central claim depends on an adopted 50 kpc distance, phenomenological blackbody fits to low-count X-ray data, the assumption that the optical continuum is purely stellar, and the interpretation of the WISE color trend as donor pulsation. Appendix D uses hand-picked disk parameters to match the observed period; these are consistency checks rather than independent evidence. No new physical entities are introduced.

free parameters (10)
  • Distance to J0431-71 = 50 kpc
    Adopted from Magellanic literature (§1); enters L_X, Mdot, R_star and orbital period as d^2. Not measured in this paper.
  • kT_bb (eRASS2) = 26^{+12}_{-8} eV
    Fitted blackbody temperature (Table 5); defines the SSS component and feeds luminosity and Mdot.
  • kT_bb (eRASS3) = 18^{+9}_{-6} eV
    Fitted blackbody temperature (Table 5); used for the bright-state luminosity.
  • kT_bb (XMM1) = 29^{+8}_{-6} eV
    Fitted blackbody temperature from the faint-state XMM observation (Table 5).
  • kT_bb (Swift Sw1) = 30 eV (frozen)
    kT fixed at 30 eV for the Swift spectrum instead of being fit.
  • Blackbody normalization / R_bbody per epoch = R_bbody 0.025-0.39 R_sun (eRASS2/3), 0.004 R_sun (XMM1)
    Fitted bbodyrad normalization; highly degenerate with kT (Appendix C). Governs the unabsorbed L_X.
  • N_H,Gal = 8.6e20 cm^-2
    Fixed Galactic absorption from Dickey & Lockman (1990); intrinsic N_H is only weakly constrained (upper limit <5e20 cm^-2).
  • M_WD for viscous timescale = 1.0 Msun
    Chosen in Appendix D, not measured; used to make t_visc consistent with the observed 524-day period.
  • alpha, H/R (slim disk) = 0.5, 0.5
    Chosen slim-disk parameters in Appendix D; with M_WD=1.0 they produce t_visc 430-634 days.
  • Bolometric correction BC_I = -2.05
    Assumed from a 3600 K blackbody (§8.3); the authors caution it is strongly model-dependent. Converts I magnitude to Lbol=1.5e4 Lsun and Rstar=337 Rsun.
axioms (7)
  • domain assumption The source distance is 50 kpc
    Section 1: 'The distance of the source is assumed to be 50 kpc'; all absolute luminosities and accretion rates scale with d^2.
  • domain assumption bbodyrad is an adequate phenomenological model for the WD atmosphere
    Section 6: 'bbodyrad can be treated as an approximate or phenomenological model for white-dwarf atmospheres'; kT and normalization are degenerate.
  • domain assumption There is no intrinsic absorption/outflow beyond Galactic N_H
    Section 6: S2 model is not preferred, but N_H is only limited to <5e20 cm^-2; low counts leave this weakly constrained.
  • domain assumption The entire optical continuum originates from the red-giant companion
    Section 7: used to fit ATLAS-T templates and infer Teff=4040 K; disk or nebular contamination would bias stellar parameters.
  • ad hoc to paper The ~524-day optical/IR periodicity is a single coherent donor pulsation
    Inferred from Lomb-Scargle over a few cycles and the WISE redder-when-brighter trend; no radial-velocity confirmation is presented.
  • domain assumption WISE W1-W2 redder-when-brighter implies a cooler, larger photosphere rather than irradiation or dust
    Section 8.3: used to reject orbital/reprocessing origins and to favor stellar pulsation.
  • ad hoc to paper Slim-disk viscous parameters adopted in Appendix D
    M_WD=1.0 Msun, alpha=0.5, H/R=0.5 are chosen so t_visc spans the observed period; not independently derived from this source's data.

pith-pipeline@v1.3.0-daily-deepseek · 23661 in / 18685 out tokens · 175737 ms · 2026-08-01T02:25:41.953036+00:00 · methodology

0 comments
read the original abstract

The Magellanic Bridge stellar population is a relic of the tidal interaction between the Large and Small Magellanic Clouds. A comprehensive view of the evolution of the Bridge stellar population requires probing the compact remnants of stellar evolution, otherwise hidden at optical wavelengths. The all-sky survey conducted by the eROSITA instrument on-board the Spectrum Roentgen Gamma observatory has discovered a significant population of compact-object-powered systems in the Bridge using X-ray. The candidate super-soft source eRASSU J043115.8-711730 (hereafter J0431-71) was discovered as a part of this campaign, and we present here a deeper study of this source using XMM-Newton and SALT spectroscopy, long-term optical-infrared photometry using OGLE, ATLAS, ASAS-SN, WISE, and GAIA data. J0431-71 is a highly variable super-soft X-ray source, classified as a red giant with the GAIA color-magnitude diagram. The source exhibits: (a) a thermal X-ray spectrum with a temperature of kT$\sim$30 eV and a bright state luminosity of $3.2\times10^37$~erg~s$^{-1}$ in the 0.15-1 keV band, (b) Balmer emission lines, [Fe X] coronal line, HeII emission, and the Bowen fluorescence blend, (c) an optical and infrared periodicity of $\sim$500-560 days in phase with the X-ray-UV emission, (d) a 'redder-when-brighter' trend in the stellar emission with a $\sim$520 day period indicating a pulsating donor star. We argue that the observed spectral and temporal properties in J0431-71 are consistent with a high-accretion rate onto a white-dwarf via Roche-lobe overflow, making J0431-71 the first symbiotic source discovered in the Bridge.

Figures

Figures reproduced from arXiv: 2607.27730 by Andrej Udalski, Chandreyee Maitra, David Buckley, David Kaltenbrunner, Frank Haberl, Itumenleng Monageng, Lee Townsend, Manami Sasaki, Mara Salvato, Philip Charles, Sara Saeedi, Tathagata Saha.

Figure 1
Figure 1. Figure 1: The four eROSITA all-sky scans demonstrating the X-ray variability of J0431–71 over two years in the 0.2–8.0 keV energy range. The red circle (radius 30′′) is centered around J0431–71. for each of the eRASS were found to exhibit total counts ranging be￾tween 166 and 190. 3.2 XMM-Newton J0431–71 has been observed with XMM-Newton (Jansen et al. 2001) on 29th August 2024: ObsID: 0941321001 (PI: C. Maitra). EP… view at source ↗
Figure 2
Figure 2. Figure 2: J0431–71 Gaia CMD for stars in LMC. The bin size for the colour (BP − RP) and magnitude (G) axes are 0.01 and 0.02 respectively. The solid lines represent boundaries between different stellar types (Gaia Collab. et al. 2021). J0431-71 is marked by the red ‘+’, and lies in the RGB region [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: LS periodogram of the original OGLE I-band light-curve of J0431–71. The LS periodogram is plotted with three period ranges for better clarity left: 2–20 days, center: 20–200 days, and right: 200–2000 days The red and black dashed lines mark the 95% and 99% confidence levels. The other peaks are artifacts of the sampling as verified with simulated light-curves (Section 5). at the OGLE observation times show… view at source ↗
Figure 4
Figure 4. Figure 4: (a) X-ray variability including the HILIGT upper-limits (see text). These fluxes are not corrected for Galactic absorption; (b) UV photometry from XMM-Newton and Swift; (c) long-term I-band photometry from OGLE; (d) ATLAS c- and o- band light-curves with a moving average of 10 d; (e) variability in WISE W1-W2 colour. The red-dashed line indicates the epoch of SALT observation. respectively. For other instr… view at source ↗
Figure 5
Figure 5. Figure 5: Convolved X-ray spectra of J0431–71 from (a) eRASS2, (b) eRASS3, (c) XMM-Newton (only EPIC-pn for clarity). The best fit source model is shown in deep blue and the best fit PCA background model is in black. The shaded regions (blue - source; grey - background) indicate 68% (darker) and 90% (lighter) confidence bands, with the confidence range calculated from BXA samples. eROSITA and XMM-Newton spectra plot… view at source ↗
Figure 6
Figure 6. Figure 6: Flux calibrated SALT RSS spectrum from 20th November 2025. The prominent emission features have been identified. The grey lines indicate SALT chip gaps between 5075–5130 Å and 6124–6180 Å. The weak [O VI] Raman-scattered line wavelengths are demarcated with the blue dotted lines [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: (a) Phased UV, X-ray, OGLE I and V-band light-curves, and WISE colour (W1 − W2), folded on the OGLE period of 524 d. The brown line (and band) represents the WISE colour (and error bar). The dashed vertical lines in all panels with respective colors indicate the epochs in phase of each X-ray and the SALT observation. (b) Cartoon schematic of the effect of stellar pulsation on the accretion rate onto the wh… view at source ↗
Figure 8
Figure 8. Figure 8: Broad band spectrum of J0431–71 extending from X-rays to NIR, with symbols identified in the box above. All fluxes are corrected for Galactic extinction. The vertical lines indicate the ionizing potential of corresponding emission lines. For XMM-Newton, only the EPIC-pn data is plotted. UVW1 bands, which appear flatter than expected from a single￾temperature blackbody with kT > 15 eV. This suggests a diffe… view at source ↗
Figure 9
Figure 9. Figure 9: Proper motions of old stars in the Magellanic Bridge region from (20◦ < α < 70◦ and −77◦ < δ < −69◦ ), see Bagheri et al. (2013), cross-matched with the GAIA DR3 catalogue filtered for LMC and SMC sources. The black circle and arrow represents the position and proper-motion of J0431–71. The Magellanic Bridge burster, eRASSt J040515.6-745202 (Haberl et al. 2023), is the red diamond, and the purple circle an… view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

174 extracted references · 29 canonical work pages · 2 internal anchors

  1. [1]

    , keywords =

    The Astropy Project: Sustaining and Growing a Community-oriented Open-source Project and the Latest Major Release (v5.0) of the Core Package. , keywords =. doi:10.3847/1538-4357/ac7c74 , archivePrefix =. 2206.14220 , primaryClass =

    Pith/arXiv arXiv

  2. [3]

    and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and

    Virtanen, Pauli and Gommers, Ralf and Oliphant, Travis E. and Haberland, Matt and Reddy, Tyler and Cournapeau, David and Burovski, Evgeni and Peterson, Pearu and Weckesser, Warren and Bright, Jonathan and. Nature Methods , year =

  3. [4]

    Hunter, J. D. , Title =. Computing in Science & Engineering , Volume =

  4. [6]

    , keywords =

    The detection of an older population in the Magellanic Bridge. , keywords =. doi:10.1051/0004-6361/201118236 , archivePrefix =. 1209.0216 , primaryClass =

    Pith/arXiv arXiv

  5. [7]

    , keywords =

    A catalogue of symbiotic stars. , keywords =. doi:10.1051/aas:2000280 , archivePrefix =. astro-ph/0005547 , primaryClass =

    Pith/arXiv arXiv

  6. [8]

    , keywords =

    Are the Magellanic Clouds on Their First Passage about the Milky Way?. , keywords =. doi:10.1086/521385 , archivePrefix =. astro-ph/0703196 , primaryClass =

    Pith/arXiv arXiv

  7. [9]

    , keywords =

    X-ray spectral modelling of the AGN obscuring region in the CDFS: Bayesian model selection and catalogue. , keywords =. doi:10.1051/0004-6361/201322971 , archivePrefix =. 1402.0004 , primaryClass =

    Pith/arXiv arXiv

  8. [10]

    The Journal of Open Source Software , keywords =

    UltraNest - a robust, general purpose Bayesian inference engine. The Journal of Open Source Software , keywords =. doi:10.21105/joss.03001 , archivePrefix =. 2101.09604 , primaryClass =

    Pith/arXiv arXiv

  9. [12]

    IPHAS and the symbiotic stars. I. Selection method and first discoveries. , keywords =. doi:10.1051/0004-6361:20078989 , archivePrefix =. 0712.2391 , primaryClass =

    Pith/arXiv arXiv

  10. [13]

    , keywords =

    The Magellanic Inter-Cloud Project (MAGIC) III: first spectroscopic evidence of a dwarf stripping a dwarf. , keywords =. doi:10.1093/mnras/stx1932 , archivePrefix =. 1707.08397 , primaryClass =

    Pith/arXiv arXiv

  11. [14]

    , keywords =

    The Tidal Origin of the Magellanic Stream and the Possibility of a Stellar Counterpart. , keywords =. doi:10.1088/0004-637X/750/1/36 , archivePrefix =. 1112.6191 , primaryClass =

    Pith/arXiv arXiv

  12. [18]

    Astronomical Data Analysis Software and Systems (ADASS) XIII , year = 2004, editor =

    The XMM-Newton SAS - Distributed Development and Maintenance of a Large Science Analysis System: A Critical Analysis. Astronomical Data Analysis Software and Systems (ADASS) XIII , year = 2004, editor =

    2004

  13. [19]

    , keywords =

    N-body simulations of the Small Magellanic Cloud and the Magellanic Stream. , keywords =. doi:10.1093/mnras/278.1.191 , archivePrefix =. astro-ph/9503095 , primaryClass =

    Pith/arXiv arXiv

  14. [21]

    , keywords =

    eRASSt J040515.6 ‒ 745202, an X-ray burster in the Magellanic Bridge. , keywords =. doi:10.1051/0004-6361/202245015 , archivePrefix =. 2211.06698 , primaryClass =

    Pith/arXiv arXiv

  15. [23]

    , keywords =

    LMC S63: a historical reappraisal of the outburst behaviour of a deeply eclipsing Magellanic symbiotic star. , keywords =. doi:10.1093/mnras/stv1215 , archivePrefix =. 1505.07740 , primaryClass =

    Pith/arXiv arXiv

  16. [24]

    , keywords =

    LMC S154: the first Magellanic symbiotic recurrent nova. , keywords =. doi:10.1051/0004-6361/201834165 , archivePrefix =. 1902.02621 , primaryClass =

    Pith/arXiv arXiv 1902

  17. [25]

    , keywords =

    Two SMC Symbiotic Stars Undergoing Steady Hydrogen Burning. , keywords =. doi:10.1086/514806 , archivePrefix =. astro-ph/0702419 , primaryClass =

    Pith/arXiv arXiv

  18. [28]

    Data Release 2: Machine-learning based classification of sources in the Southern Hemisphere

    VEXAS: VISTA EXtension to Auxiliary Surveys. Data Release 2: Machine-learning based classification of sources in the Southern Hemisphere. , keywords =. doi:10.1051/0004-6361/202040131 , archivePrefix =. 2103.09257 , primaryClass =

    Pith/arXiv arXiv

  19. [30]

    , keywords =

    The Second-Generation Guide Star Catalog: Description and Properties. , keywords =. doi:10.1088/0004-6256/136/2/735 , archivePrefix =. 0807.2522 , primaryClass =

    Pith/arXiv arXiv

  20. [31]

    , keywords =

    Symbiotic stars in X-rays. , keywords =. doi:10.1051/0004-6361/201220792 , archivePrefix =. 1211.6082 , primaryClass =

    Pith/arXiv arXiv

  21. [32]

    , keywords =

    Initial Performance of the NEOWISE Reactivation Mission. , keywords =. doi:10.1088/0004-637X/792/1/30 , archivePrefix =. 1406.6025 , primaryClass =

    Pith/arXiv arXiv

  22. [33]

    , keywords =

    A Population of Accreted Small Magellanic Cloud Stars in the Large Magellanic Cloud. , keywords =. doi:10.1088/0004-637X/737/1/29 , archivePrefix =. 1106.0044 , primaryClass =

    Pith/arXiv arXiv

  23. [34]

    , keywords =

    The eROSITA X-ray telescope on SRG. , keywords =. doi:10.1051/0004-6361/202039313 , archivePrefix =. 2010.03477 , primaryClass =

    Pith/arXiv arXiv 2010

  24. [35]

    , keywords =

    The RapidXMM upper limit server: X-ray aperture photometry of the XMM-Newton archival observations. , keywords =. doi:10.1093/mnras/stac272 , archivePrefix =. 2106.01687 , primaryClass =

    Pith/arXiv arXiv

  25. [36]

    , keywords =

    OGLE-ING the Magellanic System: Stellar Populations in the Magellanic Bridge. , keywords =. doi:10.1088/0004-637X/795/2/108 , archivePrefix =. 1405.7364 , primaryClass =

    Pith/arXiv arXiv

  26. [37]

    Its telescopes and first scientific results

    SRG X-ray orbital observatory. Its telescopes and first scientific results. , keywords =. doi:10.1051/0004-6361/202141179 , archivePrefix =. 2104.13267 , primaryClass =

    Pith/arXiv arXiv

  27. [39]

    , keywords =

    The Swift Gamma-Ray Burst Mission. , keywords =. doi:10.1086/422091 , archivePrefix =. astro-ph/0405233 , primaryClass =

    Pith/arXiv arXiv

  28. [40]

    Structure and properties of the Magellanic Clouds

    Gaia Early Data Release 3. Structure and properties of the Magellanic Clouds. , keywords =. doi:10.1051/0004-6361/202039588 , archivePrefix =. 2012.01771 , primaryClass =

    Pith/arXiv arXiv 2012

  29. [42]

    , keywords =

    The Man behind the Curtain: X-Rays Drive the UV through NIR Variability in the 2013 Active Galactic Nucleus Outburst in NGC 2617. , keywords =. doi:10.1088/0004-637X/788/1/48 , archivePrefix =. 1310.2241 , primaryClass =

    Pith/arXiv arXiv 2013

  30. [43]

    , keywords =

    Sherpa: An Open-source Python Fitting Package. , keywords =. doi:10.3847/1538-4365/ad7bab , archivePrefix =. 2409.10400 , primaryClass =

    Pith/arXiv arXiv

  31. [44]

    , keywords =

    ATLAS: A High-cadence All-sky Survey System. , keywords =. doi:10.1088/1538-3873/aabadf , archivePrefix =. 1802.00879 , primaryClass =

    Pith/arXiv arXiv

  32. [45]

    An X-Shooter campaign in the high state

    V Sge: supersoft source or exotic hot binary? ─ I. An X-Shooter campaign in the high state. , keywords =. doi:10.1093/mnras/staf1284 , archivePrefix =. 2507.22637 , primaryClass =

    Pith/arXiv arXiv

  33. [46]

    , keywords =

    Discovery of four super-soft X-ray sources in XMM-Newton observations of the Large Magellanic Cloud. , keywords =. doi:10.1051/0004-6361/202142159 , archivePrefix =. 2110.02165 , primaryClass =

    Pith/arXiv arXiv

  34. [48]

    , keywords =

    The orbital period of the symbiotic star AX Per. , keywords =. doi:10.1086/130957 , adsurl =

    doi:10.1086/130957

  35. [49]

    , keywords =

    The XMM-Newton survey of the Small Magellanic Cloud: The X-ray point-source catalogue. , keywords =. doi:10.1051/0004-6361/201219935 , archivePrefix =. 1307.7594 , primaryClass =

    Pith/arXiv arXiv

  36. [50]

    arXiv e-prints , keywords =

    Broadband study of the Be/X-ray binary pulsar eRASSU J012422.9-724248 in the Magellanic Bridge, near the Eastern Wing of the Small Magellanic Cloud. arXiv e-prints , keywords =

  37. [51]

    American Astronomical Society Meeting Abstracts , year = 2004, series =

    The Naval Observatory Merged Astrometric Dataset (NOMAD). American Astronomical Society Meeting Abstracts , year = 2004, series =

    2004

  38. [52]

    VizieR Online Data Catalog: AllWISE Data Release (Cutri+ 2013)

    2013

  39. [53]

    , keywords =

    Raman-scattered O VI Features in the Symbiotic Nova RR Telescopii. , keywords =. doi:10.3847/1538-4357/ac03b1 , archivePrefix =. 2105.09442 , primaryClass =

    Pith/arXiv arXiv

  40. [54]

    X-ray properties of symbiotic stars. II. Systems with colliding winds. , keywords =

  41. [57]

    Baltic Astronomy , keywords =

    Symbiotic Stars: Observations Confront Theory. Baltic Astronomy , keywords =. doi:10.1515/astro-2017-0352 , archivePrefix =. 1110.2361 , primaryClass =

    Pith/arXiv arXiv 2017

  42. [58]

    , keywords =

    Accreting white dwarf models for CAL 83, CAL 87 and other ultrasoft X-ray sources in the LMC. , keywords =

  43. [59]

    , keywords =

    A helium-burning white dwarf binary as a supersoft X-ray source. , keywords =. doi:10.1038/s41586-023-05714-4 , archivePrefix =. 2303.13338 , primaryClass =

    Pith/arXiv arXiv

  44. [60]

    , keywords =

    Discovery of a variable supersoft X-ray source in the Large Magellanic Cloud during the ROSAT all-sky survey. , keywords =

  45. [61]

    , keywords =

    Super-soft X-ray sources in the fields of the Magellanic Clouds. , keywords =

  46. [62]

    , keywords =

    Catalog of supersoft X-ray sources. , keywords =. doi:10.1016/S1384-1076(00)00018-X , archivePrefix =. astro-ph/0005238 , primaryClass =

    Pith/arXiv arXiv

  47. [63]

    Astronomy Reports , keywords =

    Supersoft X-ray Sources: Basic Parameters. Astronomy Reports , keywords =. doi:10.1134/1.1562214 , archivePrefix =. astro-ph/0603430 , primaryClass =

    Pith/arXiv arXiv

  48. [64]

    Astronomische Gesellschaft Abstract Series , year = 1993, series =

    Optical to X-ray spectroscopy of the galactic supersoft X-ray source RX J0019+21. Astronomische Gesellschaft Abstract Series , year = 1993, series =

    1993

  49. [65]

    The method and examples

    Multiwavelength modelling the SED of supersoft X-ray sources I. The method and examples. , keywords =. doi:10.1016/j.newast.2013.10.009 , archivePrefix =. 1401.1848 , primaryClass =

    Pith/arXiv arXiv 2013

  50. [66]

    Disentangling the composite continuum of symbiotic binaries. I. S-type systems. , keywords =. doi:10.1051/0004-6361:20034262 , archivePrefix =. astro-ph/0507272 , primaryClass =

    Pith/arXiv arXiv

  51. [68]

    , year = 1997, month = jan, volume =

    Luminous Supersoft X-Ray Sources. , year = 1997, month = jan, volume =. doi:10.1146/annurev.astro.35.1.69 , adsurl =

    doi:10.1146/annurev.astro.35.1.69 1997

  52. [69]

    X-ray catalogue

    The eROSITA Final Equatorial Depth Survey (eFEDS). X-ray catalogue. , keywords =. doi:10.1051/0004-6361/202141266 , archivePrefix =. 2106.14517 , primaryClass =

    Pith/arXiv arXiv

  53. [72]

    The Central Engine of Active Galactic Nuclei , year = 2007, editor =

    First Observations with the Southern African Large Telescope (SALT). The Central Engine of Active Galactic Nuclei , year = 2007, editor =

    2007

  54. [74]

    Instrument Design and Performance for Optical/Infrared Ground-based Telescopes , year = 2003, editor =

    Prime Focus Imaging Spectrograph for the Southern African Large Telescope: optical design. Instrument Design and Performance for Optical/Infrared Ground-based Telescopes , year = 2003, editor =. doi:10.1117/12.460312 , adsurl =

    doi:10.1117/12.460312 2003

  55. [75]

    Instrument Design and Performance for Optical/Infrared Ground-based Telescopes , year = 2003, editor =

    Prime focus imaging spectrograph for the Southern African large telescope: operational modes. Instrument Design and Performance for Optical/Infrared Ground-based Telescopes , year = 2003, editor =. doi:10.1117/12.460315 , adsurl =

    doi:10.1117/12.460315 2003

  56. [76]

    The Stellar Counterparts of eROSITA sources identified by machine learning and Bayesian algorithms

    The eROSITA Final Equatorial-Depth Survey (eFEDS). The Stellar Counterparts of eROSITA sources identified by machine learning and Bayesian algorithms. , keywords =. doi:10.1051/0004-6361/202141133 , archivePrefix =. 2106.14521 , primaryClass =

    Pith/arXiv arXiv

  57. [77]

    , keywords =

    The VizieR database of astronomical catalogues. , keywords =. doi:10.1051/aas:2000169 , archivePrefix =. astro-ph/0002122 , primaryClass =

    Pith/arXiv arXiv

  58. [79]

    Asymptotic Giant Branch Stars , year = 1999, editor =

    MACHO observations of LMC red giants: Mira and semi-regular pulsators, and contact and semi-detached binaries. Asymptotic Giant Branch Stars , year = 1999, editor =

    1999

  59. [80]

    IPHAS and the symbiotic stars. III. New discoveries and their IR spectral energy distributions. , keywords =. doi:10.1051/0004-6361/201323182 , adsurl =

    work page doi:10.1051/0004-6361/201323182

  60. [81]

    , keywords =

    An X-Ray and Optical Light Curve Model of the Eclipsing Symbiotic Binary SMC3. , keywords =. doi:10.1088/0004-637X/763/1/5 , archivePrefix =. 1211.5728 , primaryClass =

    Pith/arXiv arXiv

  61. [83]

    , keywords =

    The INT Photometric H Survey of the Northern Galactic Plane (IPHAS). , keywords =. doi:10.1111/j.1365-2966.2005.09330.x , archivePrefix =. astro-ph/0506726 , primaryClass =

    arXiv 2005

  62. [84]

    , keywords =

    Seyfert-Type Dependences of Narrow Emission-Line Ratios and Physical Properties of High-Ionization Nuclear Emission-Line Regions in Seyfert Galaxies. , keywords =. doi:10.1093/pasj/53.4.629 , archivePrefix =. astro-ph/0107025 , primaryClass =

    Pith/arXiv arXiv

  63. [85]

    , keywords =

    ORFEUS spectroscopy of the O BT VI lines in symbiotic stars and the Raman scattering process. , keywords =

  64. [86]

    Mid-infrared Selection of Active Galactic Nuclei with the Wide-Field Infrared Survey Explorer. I. Characterizing WISE-selected Active Galactic Nuclei in COSMOS. , keywords =. doi:10.1088/0004-637X/753/1/30 , archivePrefix =. 1205.0811 , primaryClass =

    Pith/arXiv arXiv

  65. [88]

    , keywords =

    Surface Hydrogen-burning Modeling of Supersoft X-Ray Binaries: Are They Type Ia Supernova Progenitors?. , keywords =. doi:10.1086/424513 , archivePrefix =. astro-ph/0407466 , primaryClass =

    Pith/arXiv arXiv

  66. [90]

    , keywords =

    XZ: Deriving redshifts from X-ray spectra of obscured AGN. , keywords =. doi:10.1051/0004-6361/201833412 , archivePrefix =. 1807.01782 , primaryClass =

    Pith/arXiv arXiv

  67. [91]

    Astronomische Nachrichten , keywords =

    Accreting white dwarfs as supersoft X-ray sources. Astronomische Nachrichten , keywords =. doi:10.1002/asna.200911315 , archivePrefix =. 0909.1497 , primaryClass =

    Pith/arXiv arXiv

  68. [92]

    , keywords =

    Prediction of the Supersoft X-Ray Phase, Helium Enrichment, and Turnoff Time in the 2000 Outburst of the Recurrent Nova Ci Aquilae. , keywords =. doi:10.1086/320693 , archivePrefix =. astro-ph/0104461 , primaryClass =

    Pith/arXiv arXiv 2000

  69. [94]

    Observational appearance

    Black holes in binary systems. Observational appearance. , year = 1973, month = jan, volume =

    1973

  70. [95]

    , keywords =

    The origin of the supersoft X-ray-optical/UV flux anticorrelation in the symbiotic binary AG Draconis. , keywords =. doi:10.1051/0004-6361/200811418 , archivePrefix =. 0908.1624 , primaryClass =

    Pith/arXiv arXiv

  71. [98]

    , keywords =

    The Orbital Nature of 81 Ellipsoidal Red Giant Binaries in the Large Magellanic Cloud. , keywords =. doi:10.3847/1538-4357/835/2/209 , archivePrefix =. 1702.02376 , primaryClass =

    Pith/arXiv arXiv

  72. [99]

    , keywords =

    A comprehensive Gaia view of ellipsoidal and rotational red giant binaries. , keywords =. doi:10.1051/0004-6361/202453394 , archivePrefix =. 2502.11667 , primaryClass =

    Pith/arXiv arXiv

  73. [103]

    , keywords =

    The origin of the microlensing events observed towards the LMC and the stellar counterpart of the Magellanic stream. , keywords =. doi:10.1093/mnras/sts192 , archivePrefix =. 1205.4724 , primaryClass =

    Pith/arXiv arXiv

  74. [104]

    , keywords =

    Understanding the Lomb-Scargle Periodogram. , keywords =. doi:10.3847/1538-4365/aab766 , archivePrefix =. 1703.09824 , primaryClass =

    Pith/arXiv arXiv

  75. [106]

    , keywords =

    Radiation pressure and pulsation effects on the Roche lobe. , keywords =. doi:10.1051/0004-6361/200912313 , archivePrefix =. 0907.1229 , primaryClass =

    Pith/arXiv arXiv

  76. [107]

    First X-ray catalogues and data release of the western Galactic hemisphere

    The SRG/eROSITA all-sky survey. First X-ray catalogues and data release of the western Galactic hemisphere. , keywords =. doi:10.1051/0004-6361/202347165 , archivePrefix =. 2401.17274 , primaryClass =

    Pith/arXiv arXiv

  77. [108]

    , keywords =

    Depth estimation of the Large and Small Magellanic Clouds. , keywords =. doi:10.1051/0004-6361/200811029 , archivePrefix =. 0809.4362 , primaryClass =

    Pith/arXiv arXiv

  78. [110]

    Aaronson M., Mould J., 1985, @doi [ ] 10.1086/162973 , https://ui.adsabs.harvard.edu/abs/1985ApJ...290..191A 290, 191

    doi:10.1086/162973 1985

  79. [111]

    A., Czerny B., Lasota J

    Abramowicz M. A., Czerny B., Lasota J. P., Szuszkiewicz E., 1988, @doi [ ] 10.1086/166683 , https://ui.adsabs.harvard.edu/abs/1988ApJ...332..646A 332, 646

    doi:10.1086/166683 1988

  80. [112]

    Astropy Collaboration et al., 2022, @doi [ ] 10.3847/1538-4357/ac7c74 , https://ui.adsabs.harvard.edu/abs/2022ApJ...935..167A 935, 167

    doi:10.3847/1538-4357/ac7c74 2022

Showing first 80 references.