pith. sign in

arxiv: 2606.25623 · v1 · pith:HQAFVNW2new · submitted 2026-06-24 · 🌌 astro-ph.SR · astro-ph.GA

New Online Database of Symbiotic Variables: Catalog and Statistical Overview of Symbiotic Binaries

Jaroslav Merc , Rudolf G\'alis , Marek Wolf This is my paper

Pith reviewed 2026-06-25 19:19 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.GA
keywords symbiotic starssymbiotic binariescatalogdatabasestellar populationsbinary systemsMilky Wayorbital parameters
0
0 comments X

The pith

A new online database catalogs nearly 1400 symbiotic variables and presents a statistical overview of the confirmed population.

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

The paper introduces the New Online Database of Symbiotic Variables as a public catalog that gathers previously scattered information on symbiotic binaries in the Milky Way and nearby galaxies. It classifies nearly 1400 objects into confirmed symbiotic stars, three categories of candidates, and misidentified sources while recording photometric, spectroscopic, orbital, and auxiliary data such as emission lines and outburst activity. A statistical overview of the confirmed population is derived from this compilation, showing distributions of orbital parameters and properties of the cool giants and hot companions. The database is positioned as a dynamic resource that supports future observational and theoretical work on these systems. Its value rests on making heterogeneous literature data accessible in one place for population-level analysis.

Core claim

NODSV contains nearly 1400 objects classified into confirmed symbiotic stars, three categories of candidates, and misidentified sources. Based on the collected data, though originating from heterogeneous studies, a statistical overview of the confirmed symbiotic population is presented, highlighting the distributions of orbital parameters and the properties of the cool giants and their hot companions.

What carries the argument

The New Online Database of Symbiotic Variables (NODSV), a publicly accessible catalog that systematically compiles photometric, spectroscopic, orbital, and auxiliary diagnostic information on symbiotic binaries from the literature.

Load-bearing premise

The data compiled from heterogeneous studies is sufficiently consistent, complete, and accurately classified to support a meaningful statistical overview of the symbiotic population.

What would settle it

A targeted re-observation campaign of a statistically significant subset of the confirmed objects that finds a high rate of objects lacking the defining emission-line or binary signatures of symbiotic stars.

Figures

Figures reproduced from arXiv: 2606.25623 by Jaroslav Merc, Marek Wolf, Rudolf G\'alis.

Figure 1
Figure 1. Figure 1: Distribution of symbiotic stars in our Galaxy. Confirmed, likely, possible and suspected symbiotic stars are denoted by blue full dots, blue empty dots, red full squares, and red empty squares, respectively. Misclassified objects are not shown. The green line represents the equator of the Milky Way. The concentration towards the galactic plane/bulge is well visible. Although the census of confirmed objects… view at source ↗
Figure 2
Figure 2. Figure 2: Distribution of orbital periods for all confirmed symbiotic stars. S-, D-, and D’-type systems are shown in yellow, dark red, and cyan, respectively. A few objects with periods longer than 5 500 days are not shown. The vertical red dashed line marks the median period of S-type systems (698 days). The reliability of period estimates depends strongly on the subtype. For S- and D’-type systems, orbital pe￾rio… view at source ↗
Figure 4
Figure 4. Figure 4: Masses of binary components in confirmed symbi￾otic stars. Upper panel: Masses of symbiotic giants (gray). The vertical red dashed line indicates the median value of 1.5 M⊙. Systems showing recurrent nova outbursts, includ￾ing V407 Cyg, are shown in dark green. Lower panel: Distribution of symbiotic white dwarf masses (gray). The vertical red dashed line marks the median value of 0.6 M⊙. Systems with recur… view at source ↗
Figure 3
Figure 3. Figure 3: Cool components of confirmed symbiotic stars. Upper panel: Distribution of spectral types. S-, D-, and D’-type systems are shown in yellow, dark red, and cyan, respectively. Middle panel: Distribution of metallicities of symbiotic giants. S-type systems with M-type giants are shown in yellow, K-type giants in olive, and D’-type sys￾tems (G giants) in cyan. Vertical red dashed lines indicate the median valu… view at source ↗
Figure 5
Figure 5. Figure 5: ). In accreting-only systems, the white dwarfs are cooler (< 105 K) and less luminous (∼ 1–102 L⊙). These estimates should be treated with caution, as the temper￾atures are sometimes only lower limits derived from the maximum observed ionization potential (U. Murset & H. Nussbaumer 1994), very often from the presence of Raman-scattered O VI lines (with ionization potential of 114 eV; see lower panel of [P… view at source ↗
read the original abstract

We present the New Online Database of Symbiotic Variables (NODSV), a comprehensive and publicly accessible catalog of known and candidate symbiotic stars in the Milky Way and nearby galaxies. The database provides an up-to-date census of confirmed symbiotic binaries and systematically compiles information previously scattered across the literature, including photometric and spectroscopic properties, orbital parameters, and characteristics of both their cool and hot stellar components. It further records auxiliary diagnostics such as detected emission lines, flickering, X-ray emission, jets, or information about outburst activity. In its current release, NODSV contains nearly 1 400 objects, classified into confirmed symbiotic stars, three categories of candidates, and misidentified sources. Based on the collected data, though originating from heterogeneous studies, we present a statistical overview of the confirmed symbiotic population, highlighting the distributions of orbital parameters and the properties of the cool giants and their hot companions. Designed as a dynamic and evolving resource, NODSV provides a foundation for future observational campaigns and theoretical investigations of symbiotic binaries.

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.

Referee Report

2 major / 2 minor

Summary. The paper presents the New Online Database of Symbiotic Variables (NODSV), a publicly accessible catalog compiling nearly 1400 confirmed symbiotic stars, candidates, and misidentified sources from the literature, including photometric, spectroscopic, orbital, and component properties plus auxiliary diagnostics. It additionally provides a statistical overview of the confirmed population's orbital parameters and the properties of cool giants and hot companions, while positioning the database as a dynamic resource for future work.

Significance. A well-curated, public database of this scale would be a useful community resource for symbiotic binary research, particularly if it enables targeted follow-up and reduces duplication of literature searches. The statistical overview, however, adds limited new insight if it simply aggregates heterogeneous literature values without demonstrated controls for classification inconsistencies or selection biases.

major comments (2)
  1. [abstract and statistical overview section] The description of data compilation and the statistical overview (abstract and the section presenting population statistics) does not specify any standardization protocols, cross-validation steps against primary sources, or quantitative handling of classification inconsistencies across the heterogeneous input studies. This directly affects the reliability of the reported distributions of orbital periods, component properties, and category assignments.
  2. [statistical overview section] No quantitative assessment of completeness, selection effects, or uncertainty propagation is provided for the confirmed symbiotic sample or the candidate categories, despite the abstract's explicit acknowledgment that the data originate from heterogeneous studies. This omission is load-bearing for any claim that the overview reflects intrinsic population properties rather than literature artifacts.
minor comments (2)
  1. [catalog description] Clarify the exact criteria used to assign objects to the three candidate categories versus confirmed or misidentified, ideally with a table or flowchart.
  2. [database documentation] Ensure all database fields are explicitly defined in the text or supplementary material so users can reproduce the statistical plots from the released data.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive comments on the NODSV manuscript. We address the major comments point by point below and have revised the manuscript to improve clarity on data compilation and the scope of the statistical overview.

read point-by-point responses

  1. Referee: [abstract and statistical overview section] The description of data compilation and the statistical overview (abstract and the section presenting population statistics) does not specify any standardization protocols, cross-validation steps against primary sources, or quantitative handling of classification inconsistencies across the heterogeneous input studies. This directly affects the reliability of the reported distributions of orbital periods, component properties, and category assignments.

    Authors: The NODSV is explicitly a literature compilation, and the values (including classifications and parameters) are reported as given in the source papers without imposing new standardization. In the revised manuscript we have expanded the data compilation section to list the primary literature sources consulted, describe the aggregation workflow, and note instances where multiple references were compared for a given object. We have also added explicit language in the statistical overview clarifying that no quantitative corrections for classification inconsistencies were applied and that the reported distributions reflect the heterogeneous literature sample as compiled. revision: partial

  2. Referee: [statistical overview section] No quantitative assessment of completeness, selection effects, or uncertainty propagation is provided for the confirmed symbiotic sample or the candidate categories, despite the abstract's explicit acknowledgment that the data originate from heterogeneous studies. This omission is load-bearing for any claim that the overview reflects intrinsic population properties rather than literature artifacts.

    Authors: We agree that the overview is descriptive of the compiled sample and does not constitute a bias-corrected population study. The revised text now states in both the abstract and the statistical overview section that the distributions should be interpreted as reflecting the current heterogeneous literature compilation rather than intrinsic properties, and we explicitly caution readers about selection effects and incompleteness. A full quantitative treatment of completeness, selection biases, and uncertainty propagation lies outside the scope of a catalog paper; the database is instead intended as a resource to enable such analyses in future work. revision: yes

Circularity Check

0 steps flagged

No circularity: pure data compilation with descriptive statistics

full rationale

The paper compiles literature data into a catalog (NODSV) and presents descriptive statistics on orbital parameters and component properties. No equations, fitted models, predictions, or derivations appear in the abstract or described content. The statistical overview is explicitly noted as originating from heterogeneous studies without any reduction to author-defined quantities or self-citation chains. This matches the default expectation of a non-circular catalog paper.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a literature compilation paper; no new physical parameters are fitted, no mathematical axioms are invoked beyond standard astronomical data handling, and no new entities are postulated.

pith-pipeline@v0.9.1-grok · 5709 in / 1102 out tokens · 34852 ms · 2026-06-25T19:19:29.320069+00:00 · methodology

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

115 extracted references · 98 canonical work pages · 8 internal anchors

  1. [1]

    2023, MNRAS, 519, 6044, doi: 10.1093/mnras/stad096

    Akras, S. 2023, MNRAS, 519, 6044, doi: 10.1093/mnras/stad096

    work page doi:10.1093/mnras/stad096 2023

  2. [2]

    R., Alvarez-Candal, A., & Pereira, C

    Akras, S., Gon¸ calves, D. R., Alvarez-Candal, A., & Pereira, C. B. 2021, MNRAS, 502, 2513, doi: 10.1093/mnras/stab195

    work page doi:10.1093/mnras/stab195 2021

  3. [3]

    2019, The Astrophysical Journal Supplement Series, 240, 21, doi: 10.3847/1538-4365/aaf88c

    Ramos-Larios, G. 2019, The Astrophysical Journal Supplement Series, 240, 21, doi: 10.3847/1538-4365/aaf88c

    work page doi:10.3847/1538-4365/aaf88c 2019

  4. [4]

    Akras, S., Karagiannis, A., Charalampopoulos, G., Gavras, P., & Guti´ errez-Soto, L. A. 2026, MNRAS, 546, stag105, doi: 10.1093/mnras/stag105

    work page doi:10.1093/mnras/stag105 2026

  5. [5]

    Allen, D. A. 1980, MNRAS, 192, 521, doi: 10.1093/mnras/192.3.521

    work page doi:10.1093/mnras/192.3.521 1980

  6. [6]

    Allen, D. A. 1984, Proceedings of the Astronomical Society of Australia, 5, 369 Astropy Collaboration, Robitaille, T. P., Tollerud, E. J., et al. 2013, A&A, 558, A33, doi: 10.1051/0004-6361/201322068 Astropy Collaboration, Price-Whelan, A. M., Sip˝ ocz, B. M., et al. 2018, AJ, 156, 123, doi: 10.3847/1538-3881/aabc4f Astropy Collaboration, Price-Whelan, A....

    work page doi:10.1051/0004-6361/201322068 1984

  7. [7]

    E., Bromley, B

    Ball, S. E., Bromley, B. C., & Kenyon, S. J. 2025, The Open Journal of Astrophysics, 8, 122, doi: 10.33232/001c.143522 Belczy´ nski, K., Miko lajewska, J., Munari, U., Ivison, R. J., & Friedjung, M. 2000, Astronomy and Astrophysics Supplement Series, 146, 407, doi: 10.1051/aas:2000280

    work page doi:10.33232/001c.143522 2025

  8. [8]

    Bidelman, W. P. 1954, ApJS, 1, 175, doi: 10.1086/190007

    work page doi:10.1086/190007 1954

  9. [9]

    A., & Rodriguez, J

    Bodaghee, A., Rahoui, F., Tomsick, J. A., & Rodriguez, J. 2012, ApJ, 751, 113, doi: 10.1088/0004-637X/751/2/113

    work page doi:10.1088/0004-637x/751/2/113 2012

  10. [10]

    Boffin, H. M. J., & Merc, J. 2025, arXiv e-prints, arXiv:2508.01304, doi: 10.48550/arXiv.2508.01304

    work page doi:10.48550/arxiv.2508.01304 2025

  11. [11]

    Boyarchuk, A. A. 1969, Commmunications of the Konkoly Observatory Hungary, 65, 395

    1969

  12. [12]

    F., Eyres, S

    Brocksopp, C., Bode, M. F., Eyres, S. P. S., et al. 2002, ApJ, 571, 947, doi: 10.1086/340018

    work page doi:10.1086/340018 2002

  13. [13]

    Cannon, A. J. 1920, Harvard College Observatory Circular, 221, 1 Catal´ an, S., Isern, J., Garc´ ıa-Berro, E., & Ribas, I. 2008, MNRAS, 387, 1693, doi: 10.1111/j.1365-2966.2008.13356.x

    work page doi:10.1111/j.1365-2966.2008.13356.x 1920

  14. [14]

    2025, ApJ, 987, 147, doi: 10.3847/1538-4357/addec3

    Chen, J., Wang, L., Li, Y.-B., et al. 2025, ApJ, 987, 147, doi: 10.3847/1538-4357/addec3

    work page doi:10.3847/1538-4357/addec3 2025

  15. [15]

    2016, ApJ, 823, 102, doi: 10.3847/0004-637X/823/2/102 Contreras Rojas, V., Jaque Arancibia, M., Ferreira Lopes, C

    Choi, J., Dotter, A., Conroy, C., et al. 2016, ApJ, 823, 102, doi: 10.3847/0004-637X/823/2/102 Contreras Rojas, V., Jaque Arancibia, M., Ferreira Lopes, C. E., et al. 2026, A&A, 708, A28, doi: 10.1051/0004-6361/202556429

    work page internal anchor Pith review doi:10.3847/0004-637x/823/2/102 2016

  16. [16]

    Corbet, R. H. D., Krimm, H. A., Barthelmy, S. D., et al. 2010, The Astronomer’s Telegram, 2570, 1

    2010

  17. [17]

    Corradi, R. L. M., Rodr´ ıguez-Flores, E. R., Mampaso, A., et al. 2008, A&A, 480, 409, doi: 10.1051/0004-6361:20078989

    work page doi:10.1051/0004-6361:20078989 2008

  18. [18]

    Corradi, R. L. M., Valentini, M., Munari, U., et al. 2010, A&A, 509, A41, doi: 10.1051/0004-6361/200913231

    work page doi:10.1051/0004-6361/200913231 2010

  19. [19]

    2018, ApJ, 866, 21, doi: 10.3847/1538-4357/aadfd6

    Ramirez-Ruiz, E., & Choi, J. 2018, ApJ, 866, 21, doi: 10.3847/1538-4357/aadfd6

    work page doi:10.3847/1538-4357/aadfd6 2018

  20. [20]

    2022, ApJ, 935, 36, doi: 10.3847/1538-4357/ac7c6e

    De, K., Mereminskiy, I., Soria, R., et al. 2022, ApJ, 935, 36, doi: 10.3847/1538-4357/ac7c6e

    work page doi:10.3847/1538-4357/ac7c6e 2022

  21. [21]

    C., Hinkle, K

    Fekel, F. C., Hinkle, K. H., Joyce, R. R., & Skrutskie, M. F. 2000a, AJ, 120, 3255, doi: 10.1086/316872

    work page doi:10.1086/316872

  22. [22]

    C., Hinkle, K

    Fekel, F. C., Hinkle, K. H., Joyce, R. R., & Skrutskie, M. F. 2001, AJ, 121, 2219, doi: 10.1086/319966

    work page doi:10.1086/319966 2001

  23. [23]

    C., Hinkle, K

    Fekel, F. C., Hinkle, K. H., Joyce, R. R., & Wood, P. R. 2010, AJ, 139, 1315, doi: 10.1088/0004-6256/139/4/1315

    work page doi:10.1088/0004-6256/139/4/1315 2010

  24. [24]

    C., Hinkle, K

    Fekel, F. C., Hinkle, K. H., Joyce, R. R., & Wood, P. R. 2015, AJ, 150, 48, doi: 10.1088/0004-6256/150/2/48

    work page doi:10.1088/0004-6256/150/2/48 2015

  25. [25]

    C., Hinkle, K

    Fekel, F. C., Hinkle, K. H., Joyce, R. R., & Wood, P. R. 2017, AJ, 153, 35, doi: 10.3847/1538-3881/153/1/35

    work page doi:10.3847/1538-3881/153/1/35 2017

  26. [26]

    Howarth, I. D. 2008, AJ, 136, 146, doi: 10.1088/0004-6256/136/1/146

    work page doi:10.1088/0004-6256/136/1/146 2008

  27. [27]

    2007, AJ, 133, 17, doi: 10.1086/509133

    Lebzelter, T. 2007, AJ, 133, 17, doi: 10.1086/509133

    work page doi:10.1086/509133 2007

  28. [28]

    C., Joyce, R

    Fekel, F. C., Joyce, R. R., Hinkle, K. H., & Skrutskie, M. F. 2000b, AJ, 119, 1375, doi: 10.1086/301260

    work page doi:10.1086/301260

  29. [29]

    Fleming, W. P. S., & Pickering, E. C. 1912, Annals of Harvard College Observatory, 56, 165

    1912

  30. [30]

    J., Bento, J., Bojiˇ ci´ c, I

    Frew, D. J., Bento, J., Bojiˇ ci´ c, I. S., & Parker, Q. A. 2014, MNRAS, 445, 1605, doi: 10.1093/mnras/stu1185 Gaia Collaboration, Prusti, T., de Bruijne, J. H. J., et al. 2016, A&A, 595, A1, doi: 10.1051/0004-6361/201629272 Gaia Collaboration, Vallenari, A., Brown, A. G. A., et al. 2023, A&A, 674, A1, doi: 10.1051/0004-6361/202243940 Ga lan, C., Miko laj...

    work page doi:10.1093/mnras/stu1185 2014

  31. [31]

    Gaposchkin, C. H. P. 1957, The Galactic Novae 13 Gon¸ calves, D. R., Magrini, L., de la Rosa, I. G., & Akras, S. 2015, MNRAS, 447, 993, doi: 10.1093/mnras/stu2437 Gon¸ calves, D. R., Magrini, L., Martins, L. P., Teodorescu, A. M., & Quireza, C. 2012, MNRAS, 419, 854, doi: 10.1111/j.1365-2966.2011.19749.x Gon¸ calves, D. R., Magrini, L., Munari, U., Corrad...

    work page doi:10.1093/mnras/stu2437 1957

  32. [32]

    2009, A&A, 495, 931, doi: 10.1051/0004-6361:200810052

    Gromadzki, M., & Miko lajewska, J. 2009, A&A, 495, 931, doi: 10.1051/0004-6361:200810052

    work page doi:10.1051/0004-6361:200810052 2009

  33. [33]

    Light curves of symbiotic stars in massive photomeric surveys II: S and D'-type systems

    Gromadzki, M., Miko lajewska, J., & Soszy´ nski, I. 2013, AcA, 63, 405, doi: 10.48550/arXiv.1312.6063

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1312.6063 2013

  34. [34]

    Light-curves of symbiotic stars in massive photometric surveys I: D-type systems

    Gromadzki, M., Miko lajewska, J., Whitelock, P., & Marang, F. 2009, AcA, 59, 169, doi: 10.48550/arXiv.0906.4136

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.0906.4136 2009

  35. [35]

    Harris and 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

  36. [36]

    Henize, K. G. 1976, ApJS, 30, 491, doi: 10.1086/190369

    work page doi:10.1086/190369 1976

  37. [37]

    H., Fekel, F

    Hinkle, K. H., Fekel, F. C., & Joyce, R. R. 2009, ApJ, 692, 1360, doi: 10.1088/0004-637X/692/2/1360

    work page doi:10.1088/0004-637x/692/2/1360 2009

  38. [38]

    H., Fekel, F

    Hinkle, K. H., Fekel, F. C., Joyce, R. R., et al. 2019, ApJ, 872, 43, doi: 10.3847/1538-4357/aafba5

    work page doi:10.3847/1538-4357/aafba5 2019

  39. [39]

    H., Fekel, F

    Hinkle, K. H., Fekel, F. C., Joyce, R. R., et al. 2006, ApJ, 641, 479, doi: 10.1086/500350

    work page doi:10.1086/500350 2006

  40. [40]

    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

  41. [41]

    1981, in NATO Advanced Study Institute (ASI) Series C, Vol

    Iijima, T. 1981, in NATO Advanced Study Institute (ASI) Series C, Vol. 69, Photometric and Spectroscopic Binary Systems, 517, doi: 10.1007/978-94-009-8486-8 27 I lkiewicz, K., Miko lajewska, J., Scaringi, S., et al. 2022, MNRAS, 510, 2707, doi: 10.1093/mnras/stab3637

    work page doi:10.1007/978-94-009-8486-8 1981

  42. [42]

    M., et al

    Ilkiewicz, K., Mikolajewska, J., Shara, M. M., et al. 2018, arXiv e-prints, arXiv:1811.06696. https://arxiv.org/abs/1811.06696

    Pith/arXiv arXiv 2018

  43. [43]

    2012, ApJ, 750, 5, doi: 10.1088/0004-637X/750/1/5

    Kato, M., Miko lajewska, J., & Hachisu, I. 2012, ApJ, 750, 5, doi: 10.1088/0004-637X/750/1/5

    work page doi:10.1088/0004-637x/750/1/5 2012

  44. [44]

    Kenyon, S. J. 1986, The symbiotic stars

    1986

  45. [45]

    J., & Garcia, M

    Kenyon, S. J., & Garcia, M. R. 1989, AJ, 97, 194, doi: 10.1086/114969

    work page doi:10.1086/114969 1989

  46. [46]

    J., Livio, M., Mikolajewska, J., & Tout, C

    Kenyon, S. J., Livio, M., Mikolajewska, J., & Tout, C. A. 1993, ApJL, 407, L81, doi: 10.1086/186811

    work page doi:10.1086/186811 1993

  47. [47]

    , keywords =

    Kenyon, S. J., Oliversen, N. A., Mikolajewska, J., et al. 1991, AJ, 101, 637, doi: 10.1086/115712

    work page doi:10.1086/115712 1991

  48. [48]

    O., Pelisoli, I., Koester, D., et al

    Kepler, S. O., Pelisoli, I., Koester, D., et al. 2015, MNRAS, 446, 4078, doi: 10.1093/mnras/stu2388

    work page doi:10.1093/mnras/stu2388 2015

  49. [49]

    O., Pelisoli, I., Koester, D., et al

    Kepler, S. O., Pelisoli, I., Koester, D., et al. 2016, MNRAS, 455, 3413, doi: 10.1093/mnras/stv2526

    work page doi:10.1093/mnras/stv2526 2016

  50. [50]

    2016, AJ, 151, 68, doi: 10.3847/0004-6256/151/3/68

    Kirk, B., Conroy, K., Prˇ sa, A., et al. 2016, AJ, 151, 68, doi: 10.3847/0004-6256/151/3/68

    work page doi:10.3847/0004-6256/151/3/68 2016

  51. [51]

    J., Kepler, S

    Kleinman, S. J., Kepler, S. O., Koester, D., et al. 2013, ApJS, 204, 5, doi: 10.1088/0067-0049/204/1/5

    work page doi:10.1088/0067-0049/204/1/5 2013

  52. [52]

    , keywords =

    Kniazev, A. Y., V¨ ais¨ anen, P., Whitelock, P. A., et al. 2009, MNRAS, 395, 1121, doi: 10.1111/j.1365-2966.2009.14617.x

    work page doi:10.1111/j.1365-2966.2009.14617.x 2009

  53. [53]

    G., & Postnov, K

    Kuranov, A. G., & Postnov, K. A. 2015, Astronomy Letters, 41, 114, doi: 10.1134/S1063773715040064

    work page doi:10.1134/s1063773715040064 2015

  54. [54]

    2025, A&A, 698, A155, doi: 10.1051/0004-6361/202451548 Leedj¨ arv, L., G´ alis, R., Hric, L., Merc, J., & Burmeister, M

    Merc, J. 2025, A&A, 698, A155, doi: 10.1051/0004-6361/202451548 Leedj¨ arv, L., G´ alis, R., Hric, L., Merc, J., & Burmeister, M. 2016, MNRAS, 456, 2558, doi: 10.1093/mnras/stv2807

    work page doi:10.1051/0004-6361/202451548 2025

  55. [55]

    M., Anguiano, B., Stassun, K

    Lewis, H. M., Anguiano, B., Stassun, K. G., et al. 2020, ApJL, 900, L43, doi: 10.3847/2041-8213/abb248 L¨ u, G., Yungelson, L., & Han, Z. 2006, MNRAS, 372, 1389, doi: 10.1111/j.1365-2966.2006.10947.x L¨ u, G. L., Zhu, C. H., Postnov, K. A., et al. 2012, MNRAS, 424, 2265, doi: 10.1111/j.1365-2966.2012.21395.x

    work page doi:10.3847/2041-8213/abb248 2020

  56. [56]

    B., Sokoloski, J

    Lucy, A. B., Sokoloski, J. L., Luna, G. J. M., et al. 2025, MNRAS, 543, 2292, doi: 10.1093/mnras/staf1351

    work page doi:10.1093/mnras/staf1351 2025

  57. [57]

    Luna, G. J. M., Sokoloski, J. L., Mukai, K., & Nelson, T. 2013, A&A, 559, A6, doi: 10.1051/0004-6361/201220792

    work page doi:10.1051/0004-6361/201220792 2013

  58. [58]

    Magrini, L., Corradi, R. L. M., & Munari, U. 2003, in Astronomical Society of the Pacific Conference Series, Vol. 303, Symbiotic Stars Probing Stellar Evolution, ed. R. L. M. Corradi, J. Mikolajewska, & T. J. Mahoney, 539, doi: 10.48550/arXiv.astro-ph/0208085

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0208085 2003

  59. [59]

    R., & Vajgel, B

    Magrini, L., Gon¸ calves, D. R., & Vajgel, B. 2017, MNRAS, 464, 739, doi: 10.1093/mnras/stw2389

    work page doi:10.1093/mnras/stw2389 2017

  60. [60]

    2013, in IAU Symposium, Vol

    Marigo, P. 2013, in IAU Symposium, Vol. 281, Binary Paths to Type Ia Supernovae Explosions, ed. R. Di

    2013

  61. [61]

    Orio, & M

    Stefano, M. Orio, & M. Moe, 36–43, doi: 10.1017/S1743921312014664 Medina Tanco, G. A., & Steiner, J. E. 1995, AJ, 109, 1770, doi: 10.1086/117407

    work page doi:10.1017/s1743921312014664 1995

  62. [62]

    2025, Galaxies, 13, 49, doi: 10.3390/galaxies13030049

    Merc, J. 2025, Galaxies, 13, 49, doi: 10.3390/galaxies13030049

    work page doi:10.3390/galaxies13030049 2025

  63. [63]

    G., Mathur, S., & Garc´ ıa, R

    Merc, J., Beck, P. G., Mathur, S., & Garc´ ıa, R. A. 2024, A&A, 683, A84, doi: 10.1051/0004-6361/202348116

    work page doi:10.1051/0004-6361/202348116 2024

  64. [64]

    Merc, J., & Boffin, H. M. J. 2025, A&A, 695, A61, doi: 10.1051/0004-6361/202553789

    work page doi:10.1051/0004-6361/202553789 2025

  65. [65]

    Research Notes of the American Astronomical Society , year = 2019, month = feb, volume =

    Merc, J., G´ alis, R., & Wolf, M. 2019a, Research Notes of the American Astronomical Society, 3, 28, doi: 10.3847/2515-5172/ab0429

    work page doi:10.3847/2515-5172/ab0429

  66. [66]

    2019b, Astronomische Nachrichten, 340, 598, doi: 10.1002/asna.201913662

    Merc, J., G´ alis, R., & Wolf, M. 2019b, Astronomische Nachrichten, 340, 598, doi: 10.1002/asna.201913662

    work page doi:10.1002/asna.201913662

  67. [67]

    2022, MNRAS, 510, 1404, doi: 10.1093/mnras/stab3512 14

    Merc, J., G´ alis, R., Wolf, M., et al. 2022, MNRAS, 510, 1404, doi: 10.1093/mnras/stab3512 14

    work page doi:10.1093/mnras/stab3512 2022

  68. [68]

    2026a, MNRAS, 545, staf2146, doi: 10.1093/mnras/staf2146

    Udalski, A. 2026a, MNRAS, 545, staf2146, doi: 10.1093/mnras/staf2146

    work page doi:10.1093/mnras/staf2146

  69. [69]

    2020, A&A, 644, A49, doi: 10.1051/0004-6361/202039132

    Merc, J., Miko lajewska, J., Gromadzki, M., et al. 2020, A&A, 644, A49, doi: 10.1051/0004-6361/202039132

    work page doi:10.1051/0004-6361/202039132 2020

  70. [70]

    Merrill, P. W. 1958, in Liege International Astrophysical

    1958

  71. [71]

    Orbital and stellar parameters of symbiotic stars

    Colloquia, Vol. 8, Liege International Astrophysical Colloquia, 436–448 Miko lajewska, J. 2003, in Astronomical Society of the Pacific Conference Series, Vol. 303, Symbiotic Stars Probing Stellar Evolution, ed. R. L. M. Corradi, J. Mikolajewska, & T. J. Mahoney, 9, doi: 10.48550/arXiv.astro-ph/0210489 Miko lajewska, J. 2007, Baltic Astronomy, 16, 1

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.astro-ph/0210489 2003

  72. [72]

    Symbiotic Novae

    Mikolajewska, J. 2010, arXiv e-prints, arXiv:1011.5657, doi: 10.48550/arXiv.1011.5657 Miko lajewska, J. 2012, Baltic Astronomy, 21, 5, doi: 10.1515/astro-2017-0352

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1011.5657 2010

  73. [73]

    1997, A&A, 327, 191 Miko lajewska, J., Caldwell, N., & Shara, M

    Mikolajewska, J., Acker, A., & Stenholm, B. 1997, A&A, 327, 191 Miko lajewska, J., Caldwell, N., & Shara, M. M. 2014a, MNRAS, 444, 586, doi: 10.1093/mnras/stu1480 Miko lajewska, J., Ga lan, C., Hinkle, K. H., Gromadzki, M., & Schmidt, M. R. 2014b, MNRAS, 440, 3016, doi: 10.1093/mnras/stu492 Miko lajewska, J., & Shara, M. M. 2017, ApJ, 847, 99, doi: 10.384...

    work page doi:10.1093/mnras/stu1480 1997

  74. [74]

    2014, MNRAS, 440, 1410, doi: 10.1093/mnras/stu292

    Miszalski, B., & Miko lajewska, J. 2014, MNRAS, 440, 1410, doi: 10.1093/mnras/stu292

    work page doi:10.1093/mnras/stu292 2014

  75. [75]

    2013, MNRAS, 432, 3186, doi: 10.1093/mnras/stt673

    Miszalski, B., Miko lajewska, J., & Udalski, A. 2013, MNRAS, 432, 3186, doi: 10.1093/mnras/stt673

    work page doi:10.1093/mnras/stt673 2013

  76. [76]

    M., & Vogel, M

    Muerset, U., Nussbaumer, H., Schmid, H. M., & Vogel, M. 1991, A&A, 248, 458

    1991

  77. [77]

    Mukai, K., Luna, G. J. M., Cusumano, G., et al. 2016, MNRAS, 461, L1, doi: 10.1093/mnrasl/slw087

    work page doi:10.1093/mnrasl/slw087 2016

  78. [78]

    Analysis of the Gaia DR3 planetary nebula candidates and the possible symbiotic stars among them

    Mulato, L., Merc, J., Charbonnel, S., et al. 2026, arXiv e-prints, arXiv:2604.24730, doi: 10.48550/arXiv.2604.24730

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2604.24730 2026

  79. [79]

    arXiv e-prints , keywords =

    Munari, U. 2019, arXiv e-prints, arXiv:1909.01389, doi: 10.48550/arXiv.1909.01389

    work page doi:10.48550/arxiv.1909.01389 2019

  80. [80]

    2013, A&A, 558, A2, doi: 10.1051/0004-6361/201321883

    Maitan, A. 2013, A&A, 558, A2, doi: 10.1051/0004-6361/201321883

    work page doi:10.1051/0004-6361/201321883 2013

Showing first 80 references.