Pith. sign in

REVIEW 4 major objections 5 minor 2 cited by

Multiple generation star formation in Cepheus Flare

T0 review · 4 major / 5 minor · reviewed 2026-08-16 · deepseek-v4-flash

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

Pith's one-line read The Cepheus Flare region formed stars in four distinct bursts.

desk verdict A useful expanded membership catalog for ASCC 127, but the four-episode star formation history rests on isochrone ages whose systematic uncertainties are comparable to the inter-episode gaps. read the letter →

arxiv 2505.00407 v1 pith:3MCDL5C2 submitted 2025-05-01 astro-ph.SR astro-ph.GA

Fan Wang , Min Fang , Xiaoting Fu , Yang Su , Xuepeng Chen , Shiyu Zhang , Penghui Liu , Xiao-Long Wang
show 3 more authors
Haijun Tian Wenyuan Cui Zhongmu Li
This is my paper · ORCID
classification astro-ph.SRastro-ph.GA
keywords ASCC127CepheusFlaresequentialstarformationGaiaDR3movinggroupsstellarfeedbackisochroneagesinterstellarmedium
verification ladder T0 review T1 audit T2 compute T3 formal

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 argues that the nearby Cepheus Flare region did not form its stars in one event, but in at least four sequential bursts: roughly 32, 20, 15, and 7 million years ago. Using Gaia DR3 astrometry, the authors more than double the known membership of the young moving group ASCC 127, splitting it into five kinematic subgroups with distinct ages, and show that these subgroups are spatially tied to the Cepheus Flare star-forming clouds. They also identify a tens-of-parsecs cavity in the dust and gas that is expanding at about 10 km/s and would have required roughly $\sim 10^{50}$ erg to create. If the age sequence holds, the older generations' supernovae and winds likely compressed the gas and triggered the younger generations, making the region a clear case of feedback-driven, multi-generational star formation. A sympathetic reader cares because it turns a scattered young association into a laboratory for how star formation propagates through the interstellar medium.

What carries the argument

The argument rests on four linked tools. Friends-of-Friends clustering (via the ROCKSTAR code) in Gaia DR3 five-dimensional phase space (position on sky, parallax, and proper motion) expands ASCC 127 to 3,971 members; K-means then divides them into Groups 1-5. Ages come from fitting empirical color-corrected PARSEC 1.2S isochrones to dereddened color-magnitude diagrams, a correction needed because the model's low-mass main sequence is too blue. Backward orbit integrations with the MWPotential2014 model in galpy trace each group to its presumed formation site and time, connecting the age sequence to spatial positions. Finally, three-dimensional dust extinction maps plus CO and HI surveys reveal the cavity and its expansion, and a simple kinetic-energy estimate ties the cavity's $\sim 10^{50}$ erg to supernova-scale feedback. The empirical color-correction functions are the load-bearing piece for the age ladder, since without them the group ages shift by 5-6 Myr.

What would settle it

Measure independent ages for a sample of ASCC 127 members spanning all five groups using a method anchored to absolute ages, such as lithium depletion boundary fitting for M dwarfs or spectroscopic surface-gravity ages for pre-main-sequence stars. If the resulting ages for Groups 2, 3, 4, and 5 overlap within their 1-sigma uncertainties, the four-episode sequence and the feedback-triggering narrative collapse; conversely, if the 32 Myr versus 15 Myr split persists, the paper's picture is confirmed. A second check targets the cavity: high-resolution CO observations should show a clear expanding shell with a kinematic center coinciding with the older groups; absence of such a shell would weaken the feedback interpretation.

Watch

Extended reading notes

Core claim

The paper's central claim is that ASCC 127, previously treated as a single young moving group, is actually a composite of five subgroups (Groups 1-5) with best-fit isochrone ages of 32, 22, 15, 15, and 20 Myr, and that these subgroups together with the local young stellar objects (~7 Myr) record four distinct star formation episodes in the Cepheus Flare region. Backward orbit integrations place the subgroups within about 100 pc of one another at their formation times, and the oldest group formed while the others had not yet appeared. The paper further claims that a large cavity seen in dust, CO, and HI maps is an expanding structure produced by feedback from these earlier generations, and that the Loop III and Cepheus Flare Shell features are consistent with supernova-driven energy input. In the author's telling, the spatial age gradient — older groups outside, younger YSOs along an arc inside the cavity — is direct evidence that feedback from massive stars in earlier generations compressed the interstellar medium and triggered the later ones.

Load-bearing premise

The entire four-episode sequence depends on the assumption that the photometric ages from color-corrected PARSEC isochrones faithfully separate Groups 1-5 and the YSOs into distinct epochs; the age differences between groups (5-13 Myr) are comparable to the paper's own color-correction shift (5-6 Myr) and to the uncertainty of its rough 50 Myr field-star cut.

Editorial extensions

If this is right

  • ASCC 127's membership is roughly double the previous census, and its internal structure includes two newly identified subgroups, so any future study of this moving group must account for five kinematically distinct components.
  • If the age sequence is real, the Cepheus Flare YSO population at ~7 Myr is a fourth generation, and its spatial position along the arc of Group 4 indicates star formation propagating along a compressed filament.
  • The cavity's expansion time of 3-5 Myr and energy of $\sim 10^{50}$ erg imply at least one supernova from a roughly 9-solar-mass star in the older groups, consistent with the presence of Loop III and the Cepheus Flare Shell.
  • The traceback places Groups 2-5 within 60-100 pc of each other at formation, meaning the region's star formation was concentrated in a compact volume and then dispersed to the present configuration.
  • The method — combining Gaia membership, isochrone ages, orbit traceback, and ISM maps — can be applied to other nearby young associations to test whether multi-episode, feedback-triggered histories are common.

Reading between the lines

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

  • A natural test the paper leaves implicit: independent age indicators such as lithium depletion or rotation-based gyrochronology for a few dozen members of Groups 2-5 would separate systematic isochrone error from the true age spread; if those ages converge, the four-episode sequence stands, and if they overlap, it collapses.
  • The age gap between the 15 Myr Groups 3/4 and the ~7 Myr YSOs nearly matches the cavity's 3-5 Myr expansion time plus a free-fall time, so the current episode may still be ongoing and the cavity itself may host the next generation — a prediction that future submillimeter observations of dense cores inside the cavity could check.
  • Because the color correction shifts ages by 5-6 Myr while the quoted inter-group age differences are 5-13 Myr, the sequence's robustness hinges on the correction being accurate at the low-mass end; applying the same correction to a coeval benchmark cluster would directly bound this systematic.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

4 major / 5 minor

Summary. The paper re-derives the membership of the young moving group ASCC 127 from Gaia DR3, expanding it to 3,971 stars with a Friends-of-Friends algorithm and then splitting the sample into five subgroups (Groups 1–5) by K-means clustering. Ages are obtained by fitting color-corrected PARSEC 1.2S isochrones to dereddened Gaia CMDs, yielding 32, 22, 15, 15, and 20 Myr for Groups 1–5. The subgroups are compared with the known YSO population of the Cepheus Flare region, and a dust/CO/HI cavity is identified. The authors interpret the combined age ladder (32, ~20, 15, ~7 Myr) as four sequential star formation episodes, with feedback from older generations shaping the surrounding ISM and triggering later generations. The paper also presents backward orbit integrations of the five groups to support the spatial relationships among the episodes.

Significance. If the age ladder and the membership decontamination are reliable, the paper would provide a useful expanded census of ASCC 127 and a plausible case for sequential, feedback-driven star formation in the Cepheus Flare. The authors deserve credit for releasing the full membership table in machine-readable form, for applying an externally calibrated empirical color correction rather than an ad hoc one, and for combining Gaia astrometry with dust, CO, and HI data. The spatial association of the groups with Cepheus Flare clouds and the expanding cavity are interesting observational findings in their own right. However, the central multi-episode claim depends on age differences of only 5–13 Myr, and the paper's own systematic-age diagnostics (corrected vs uncorrected ages, YSO ages) cast doubt on whether those differences are currently resolved.

major comments (4)
  1. [§3.4, Table 2, footnote] The four-episode chronology rests on age differences of 5–13 Myr, but the paper's own comparison of corrected and uncorrected PARSEC ages shows a systematic shift of about 5–6 Myr (26→32, 17→22, 10→15, 10→15, 14→20 Myr). The quoted bootstrap uncertainties (1–4 Myr) measure only resampling scatter and do not include the Wang et al. (2025) empirical correction calibration, the fixed solar metallicity, STILISM extinction errors, or the 'rather rough' 50 Myr field-star cut admitted in §3.2. A systematic shift of only ~5 Myr would merge the 20 and 15 Myr episodes. The authors should quantify this systematic error budget and show that the episode spacing survives it.
  2. [§4.2, Figure 9] The 7 Myr 'episode' is not secure. The same isochrone-fitting procedure returns ~7 Myr for YSOs that Szilágyi et al. (2021) dated at 1–5 Myr, which suggests a systematic offset at the young end. Moreover, §4.2 splits Group 4 into YSOs at 7 Myr and other members at 19 Myr, while Table 2 lists a single 15 Myr age for Group 4; one episode is therefore already a blend. The authors need to reconcile these numbers and to validate the young-age scale with an independent clock before adding 7 Myr as a separate generation.
  3. [§4.2, cavity energetics] The supernova interpretation of the cavity is not supported by the paper's own stellar lifetimes. With a 9 M⊙ lifetime of ~31 Myr, a 9 M⊙ star formed in a 15–22 Myr old group has not yet exploded; Group 1 (32 Myr) would contain at most ~3 M⊙ stars. The text first states that Groups 2–5 can provide less than 10^49 erg of wind energy before their supernova explosions and then concludes that a ~10^50 erg cavity was likely produced by a supernova in these groups. The authors should either identify a specific massive member with sufficient remaining or lapsed lifetime, or soften the supernova claim to a hypothesis that is consistent with the group ages.
  4. [§3.2–§3.3] The membership selection may bias the age ladder. The 50 Myr isochrone cut is described as 'rather rough,' and an additional 169 stars are removed from Group 3 post hoc using the tangential-velocity distribution. Because the same photometry is later used to fit ages, a selection that preferentially keeps or removes young-looking stars can change the derived age sequence. The authors should quantify how the derived ages of Groups 1–5 shift under reasonable variations of the field-star cuts (e.g., 40 Myr versus 60 Myr) and under the Pang et al. (2022) membership.
minor comments (5)
  1. [Table 2 caption] There is a typo in the table caption: 'medain radial velocity' should be 'median radial velocity.'
  2. [§3.2 footnotes] The footnote reads 'the local standrd of rest' rather than 'the local standard of rest'; please fix this typo.
  3. [§4.1] The text says Groups 2 and 5 formed approximately 17 Myr after Group 1, but Table 2 gives age differences of 10–12 Myr between these groups; please clarify or correct this inconsistency.
  4. [§4.1] The paragraph describing the orbit uncertainty repeats the sentence 'We then derive the median orbit from the sampled trajectories and use the 1σ standard deviation...' twice; one copy should be removed.
  5. [§4.2 vs Table 2] The age reported for Group 4 is 15 Myr in Table 2 but 19 Myr for its non-YSO members in §4.2; these values should be reconciled in the text.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the episodic ages are externally calibrated isochrone fits, and the traceback uses those ages rather than producing them.

full rationale

The claimed derivation chain is not circular. Membership and subgrouping (Sections 3.1-3.3) are performed in kinematic and distance space using FoF and K-means without feeding photometric ages into the grouping, so the age ladder is an output rather than a selection input. The age estimates in Section 3.4 use PARSEC 1.2S isochrones with empirical color corrections taken from Wang et al. (2025); that cited calibration is external to this paper, being derived from fits to the Hyades, Pleiades, and Praesepe benchmark clusters, so adopting it is independent support rather than a self-referential loop even though authors overlap. The 'four distinct age groups' (32, 20, 15, and 7 Myr) are a restatement of the fitted group ages and the re-fitted YSO age; the paper presents them as inferred evidence, not as an independent prediction forced by construction. The backward orbit integrations simply propagate these fitted ages and observed kinematics through MWPotential2014; they do not generate the ages from the orbits. The paper's own caution that the 50 Myr field-star cut is 'rather rough' and the 5-6 Myr color-correction shifts are systematic-uncertainty concerns, not evidence that any quantity was defined in terms of the conclusion. No equation sets a fitted parameter equal to a claimed prediction, and no load-bearing uniqueness theorem is imported from the authors' prior work. Score 0.

Assumptions & free parameters 4 free parameters · 5 assumptions · 0 invented entities

The central claims rest on externally calibrated isochrone colors, a rough field-star cut, an assumed number of kinematic subgroups, and an assumed dynamical model. No new physical entities are introduced; the five subgroups and the cavity are groupings of observed stars and gas.

free parameters (4)
  • Empirical color correction functions for PARSEC 1.2S isochrones = Not re-fitted; adopted from Wang et al. (2025)
    Ages and masses of all groups and the YSOs are derived from these corrected isochrones. The correction shifts ages by 5-6 Myr, comparable to the age gaps that define the four episodes, so it is a key fitted input.
  • Number of subgroups K = 5
    K-means is run with K=5 with no presented cluster validation. The grouping into five subgroups is the foundation of the age sequence and all subsequent interpretation.
  • Adopted distance for cavity gas mass = 300 pc
    Section 4.2 computes gas mass and kinetic energy at a single distance of 300 pc while the region spans 300-500 pc. The energy scales with the assumed distance and directly affects the supernova comparison.
  • Cavity expansion velocity V_exp = ~10 km/s
    Read from the position-velocity diagram. Ekin scales as V_exp^2, so an error of a factor 2 changes the derived energy by 4, yet no uncertainty is quoted.
assumptions (5)
  • domain assumption The Wang et al. (2025) color correction, calibrated on Hyades, Pleiades, and Praesepe, is transferable to ASCC 127 and Cepheus Flare YSOs.
    Used for all age and mass estimates in Section 3.4 and for the YSO ages in Section 4.2.
  • ad hoc to paper The 50 Myr isochrone cleanly separates ASCC 127 members from field stars in the dereddened color-magnitude diagram.
    Section 3.2: all sources below this isochrone are removed as field stars. The authors themselves call the selection 'rather rough.' This cut can remove genuine older members and bias the derived age distribution.
  • domain assumption The parent molecular clouds had initial kinematics similar to those of the young groups at their formation times.
    Section 4.1, stated explicitly when estimating the trajectories of the parent clouds. If the clouds moved differently, the inferred spatial clustering of formation sites is unreliable.
  • standard math MWPotential2014 is an adequate Galactic potential for 32 Myr backward orbit integrations.
    Section 4.1: this is the standard galpy potential, but the resulting trajectories depend on the potential model and the adopted solar motion and position.
  • domain assumption The Friends-of-Friends grouping in 5D phase space with radial velocities set to zero recovers the true kinematic structure of ASCC 127.
    Section 3.2: radial velocities are not used in the initial FOF, only for the subset of 764 stars in the K-means grouping. If the group is not kinematically coherent in RV, the membership could be contaminated.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Multiple generation star formation in Cepheus Flare." pith.science (2026). https://pith.science/paper/3MCDL5C2

@misc{pith2026250500407,
  author       = {Pith},
  title        = {Pith review of: Multiple generation star formation in Cepheus Flare},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3MCDL5C2}},
  note         = {Machine review of arXiv:2505.00407}
}
read the original abstract

We present an analysis of the young stellar moving group ASCC 127 using Gaia DR3 data, significantly expanding its membership to 3,971 stars -- double the number identified in previous studies. Using kinematic and distance criteria, ASCC 127 is divided into five subgroups (Groups 1-5) with ages spanning from 15 to 32 Myr. Groups 1-5 are spatially linked to the Cepheus Flare star-forming region, revealing potential evidence of four sequential star formation episodes at approximately 32 Myr, 20 Myr, 15 Myr, and 7 Myr. Through dust and gas mapping, we identify a spatial cavity extending several tens of parsecs, which may have resulted from feedback processes such as supernovae associated with earlier generations of stars in the region. This structure, along with the larger Loop III feature, indicates that feedback from massive stars likely influenced the interstellar medium (ISM). By integrating young stellar populations with ISM studies, we provide a detailed picture of the feedback-driven star formation history in the Cepheus Flare region.

Figures

Figures reproduced from arXiv: 2505.00407 by the authors.

Figure 1
Figure 1. Distributions of 5,450 member candidates (black dots), identified by the Friends-of-Friends (FoF) algorithm, in five-parameter space (Galactocentric coordinate (ℓ, b), parallax, tangential velocity (vℓ, vb)) and the CMD (MG vs. BP−RP). has been observed in prior researches that the low-mass segment of the PARSEC 1.2S isochrones does not align well with the photometric observations of stellar groups when plotted on c… view at source ↗
Figure 2
Figure 2. Comparison the 5,450 member candidates with the field stars in this region. The left subplot: the density map of the 5,450 member candidates. The right subplot: the density map of the field stars in this region. The red dashed line is the corrected-color isochrone from PARSEC model with an age of 50 Myr and solar metallicity ([M/H]=0). 0 1 2 3 4 BP RP 2 0 2 4 6 8 10 12 M G [M/H]=0.0, 50Myr [PITH_FULL_IMAGE:figures/… view at source ↗
Figure 3
Figure 3. [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figures from the paper (7 more)
Figure 5
Figure 5. Figure 5: Distribution of Groups 1−5 in the Galactocentric coordinate (ℓ, b), parallax, tangential velocity (vℓ, vb). In all of the panels, green dots, hotpink dots, red dots, orange dots and blue dots represent the candidate members of Group 1, Group 2, Group 3, Group 4 and Gro…
Figure 6
Figure 6. Figure 6: CMDs for Groups 1−5 (same color-coding as in [PITH_FULL_IMAGE:figures/full_fig_p007_6.png]
Figure 7
Figure 7. Figure 7: 2D trajectory plot (X, Y ) of the backwards orbit integrations of Groups 1−5, tracing their motion from the past (32 Myr ago) to the present in Heliocentric Cartesian coordinates (X, Y , Z). The open circle with a dotted outline represents that the group had not yet fo…
Figure 8
Figure 8. Figure 8: Dust extinction map from Edenhofer et al. (2024), displayed in Galactic coordinates. The black dashed circle marks the Cepheus Flare Shell, provided by Kun et al. (2009), and the black solid circle indicates Loop III, provided by Kun (2007). The black dashed rectangle …
Figure 9
Figure 9. Figure 9: CMDs for 319 nearby young stellar objects (YSOs, grey and cyan dots), including 149 YSOs (cyan dots) that are part of Group 4. The black solid, dotted-dashed and dashed curves in each panel represent the best-fit, 50 Myr and 1 Myr PARSEC isochrones with empirical color…
Figure 10
Figure 10. Figure 10: Left panel: CO integrated intensity map (lime contour) from Dame et al. (2001), and HI integrated intensity map (gray background) from HI4PI Collaboration et al. (2016). The light-yellow line with the direction from upper-right to lower-left shows the routing of the p…
Figure 11
Figure 11. Figure 11: Position-velocity diagrams along the cavity (from upper-right to lower-left). Left panel: The lime solid line represents the velocity trend of CO along ℓ direction. Right panel: The lime solid line is the velocity trend of HI along the same direction. are estimated to…

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. CO Structures with Narrow Lines in Nearby Quiescent Regions

    astro-ph.GA 2026-08 conditional novelty 6.0 of 10

    A systematic MWISP survey finds 57 narrow-line CO structures, mostly nearby diffuse 'veil clouds' with subsonic turbulence, likely shaped by the Local Bubble and ion-neutral friction.

  2. CU-JADE: A Method for Traversing Extinction Jumps along the Line of Sight

    astro-ph.GA 2025-07 conditional novelty 5.0 of 10

    CU-JADE applies cumulative-sum change-point detection to stellar distance-extinction data to locate multiple dust layers, yielding new molecular cloud distances and an all-sky 3D extinction map extending to 4 kpc.

Reference graph

Works this paper leans on

65 extracted references · 8 canonical work pages · cited by 2 Pith papers

  1. [1]

    , " * write output.state after.block = add.period write newline

    ENTRY address archivePrefix author booktitle chapter doi edition editor eprint howpublished institution journal key month number organization pages publisher school series title misctitle type volume year version url label extra.label sort.label short.list INTEGERS output.state before.all mid.sentence after.sentence after.block FUNCTION init.state.consts ...

  2. [2]

    write newline

    " write newline "" before.all 'output.state := FUNCTION format.url url empty "" new.block "" url * "" * if FUNCTION format.eprint eprint empty "" archivePrefix empty "" archivePrefix "arXiv" = new.block " " eprint * " " * new.block " " eprint * " " * if if if FUNCTION format.doi doi empty "" " " doi * " " * if FUNCTION format.pid doi empty eprint empty ""...

  3. [3]

    ־ ;7B knKnYH赇z , WSG`uΟ Ɛ _2Z _[ XZ oK) zV=ߊ\||˝ \'3hK& 2_ ++>vvV Wӧeբoh t L)WdiB-C*#Pvs* ӓ+ :iMWƁ) Pw =Rȭ o^9 - GLȼ/R +

    thebibliography [1] 20pt REFERENCES 6pt =0pt 10pt plus 3pt =0pt =0pt =1pt plus 1pt =0pt =0pt -12pt =13pt plus 1pt =20pt =13pt plus 1pt \@M =10000 =-1.0em =0pt =0pt 0pt =0pt =1.0em @enumiv\@empty 10000 10000 `\.\@m \@noitemerr \@latex@warning Empty `thebibliography' environment \@ifnextchar \@reference \@latexerr Missing key on reference command Each refer...

    arXiv 2020

  4. [4]

    P., Tollerud , E

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

    doi:10.1051/0004-6361/201322068 2013

  5. [5]

    M., Sip o cz , B

    Astropy Collaboration , Price-Whelan , A. M., Sip o cz , B. M., et al. 2018, , 156, 123, 10.3847/1538-3881/aabc4f

    doi:10.3847/1538-3881/aabc4f 2018

  6. [6]

    Bailer-Jones , C. A. L., Rybizki , J., Fouesneau , M., Demleitner , M., & Andrae , R. 2021, , 161, 147, 10.3847/1538-3881/abd806

    doi:10.3847/1538-3881/abd806 2021

  7. [7]

    S., Wechsler , R

    Behroozi , P. S., Wechsler , R. H., & Wu , H.-Y. 2013, , 762, 109, 10.1088/0004-637X/762/2/109

    doi:10.1088/0004-637x/762/2/109 2013

  8. [8]

    Bell , C. P. M., Mamajek , E. E., & Naylor , T. 2015, , 454, 593, 10.1093/mnras/stv1981

    doi:10.1093/mnras/stv1981 2015

Show all 65 references
  1. [9]

    Berkhuijsen , E. M. 1973, , 24, 143

    1973

  2. [10]

    2015, , 216, 29, 10.1088/0067-0049/216/2/29

    Bovy , J. 2015, , 216, 29, 10.1088/0067-0049/216/2/29

    2015 doi

  3. [11]

    2012, , 427, 127, 10.1111/j.1365-2966.2012.21948.x

    Bressan , A., Marigo , P., Girardi , L., et al. 2012, , 427, 127, 10.1111/j.1365-2966.2012.21948.x

    2012

  4. [12]

    2023, , 522, 1288, 10.1093/mnras/stad608

    Brice \ n o-Morales , G., & Chanam \'e , J. 2023, , 522, 1288, 10.1093/mnras/stad608

    2023 doi

  5. [13]

    L., Elyajouri , M., & Monreal-Ibero , A

    Capitanio , L., Lallement , R., Vergely , J. L., Elyajouri , M., & Monreal-Ibero , A. 2017, , 606, A65, 10.1051/0004-6361/201730831

    2017 doi

  6. [14]

    Castellani , V., Degl'Innocenti , S., & Prada Moroni , P. G. 2001, , 320, 66, 10.1046/j.1365-8711.2001.03958.x

    2001

  7. [15]

    2019, , 632, A105, 10.1051/0004-6361/201936612

    Chen , Y., Girardi , L., Fu , X., et al. 2019, , 632, A105, 10.1051/0004-6361/201936612

    2019 doi

  8. [16]

    M., Hartmann , D., & Thaddeus , P

    Dame , T. M., Hartmann , D., & Thaddeus , P. 2001, , 547, 792, 10.1086/318388

    2001 doi

  9. [17]

    2024, , 685, A82, 10.1051/0004-6361/202347628

    Edenhofer , G., Zucker , C., Frank , P., et al. 2024, , 685, A82, 10.1051/0004-6361/202347628

    2024 doi

  10. [18]

    L., & Luhman , K

    Esplin , T. L., & Luhman , K. L. 2022, , 163, 64, 10.3847/1538-3881/ac3e64

    2022 doi

  11. [19]

    P., Offner , S

    Farias , J. P., Offner , S. S. R., Grudi \'c , M. Y., Guszejnov , D., & Rosen , A. L. 2024, , 527, 6732, 10.1093/mnras/stad3609

    2024 doi

  12. [20]

    A., Mackey , J., Grassitelli , L., Romano-D \' az , E., & Porciani , C

    Fichtner , Y. A., Mackey , J., Grassitelli , L., Romano-D \' az , E., & Porciani , C. 2024, , 690, A72, 10.1051/0004-6361/202449638

    2024 doi

  13. [21]

    Gaia Collaboration , Vallenari , A., Brown , A. G. A., et al. 2022, arXiv e-prints, arXiv:2208.00211, 10.48550/arXiv.2208.00211

    2022 doi arXiv

  14. [22]

    Y., Guszejnov , D., Hopkins , P

    Grudi \'c , M. Y., Guszejnov , D., Hopkins , P. F., Offner , S. S. R., & Faucher-Gigu \`e re , C.-A. 2021 a , , 506, 2199, 10.1093/mnras/stab1347

    2021 doi

  15. [23]

    Y., Guszejnov , D., Offner , S

    Grudi \'c , M. Y., Guszejnov , D., Offner , S. S. R., et al. 2022, , 512, 216, 10.1093/mnras/stac526

    2022 doi

  16. [24]

    Y., Kruijssen , J

    Grudi \'c , M. Y., Kruijssen , J. M. D., Faucher-Gigu \`e re , C.-A., et al. 2021 b , , 506, 3239, 10.1093/mnras/stab1894

    2021 doi

  17. [25]

    Guszejnov , D., Markey , C., Offner , S. S. R., et al. 2022, , 515, 167, 10.1093/mnras/stac1737

    2022 doi

  18. [26]

    2016, , 594, A116, 10.1051/0004-6361/201629178

    HI4PI Collaboration , Ben Bekhti , N., Fl \"o er , L., et al. 2016, , 594, A116, 10.1051/0004-6361/201629178

    2016 doi

  19. [27]

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

    2007 doi

  20. [28]

    2024, arXiv e-prints, arXiv:2409.07124, 10.48550/arXiv.2409.07124

    Kachelriess , M., & Mikalsen , V. 2024, arXiv e-prints, arXiv:2409.07124, 10.48550/arXiv.2409.07124

    2024 doi arXiv

  21. [29]

    Kalberla , P. M. W., & Haud , U. 2015, , 578, A78, 10.1051/0004-6361/201525859

    2015 doi

  22. [30]

    Kalberla , P. M. W., McClure-Griffiths , N. M., Pisano , D. J., et al. 2010, , 521, A17, 10.1051/0004-6361/200913979

    2010 doi

  23. [31]

    2022, arXiv e-prints, arXiv:2206.05902, 10.48550/arXiv.2206.05902

    Katz , D., Sartoretti , P., Guerrier , A., et al. 2022, arXiv e-prints, arXiv:2206.05902, 10.48550/arXiv.2206.05902

    2022 doi arXiv

  24. [32]

    Kerp , J., Winkel , B., Ben Bekhti , N., Fl \"o er , L., & Kalberla , P. M. W. 2011, Astronomische Nachrichten, 332, 637, 10.1002/asna.201011548

    2011 doi

  25. [33]

    C., & Skinner , M

    Kim , J.-G., Kim , W.-T., Ostriker , E. C., & Skinner , M. A. 2017, , 851, 93, 10.3847/1538-4357/aa9b80

    2017 doi

  26. [34]

    2019, , 158, 122, 10.3847/1538-3881/ab339a

    Kounkel , M., & Covey , K. 2019, , 158, 122, 10.3847/1538-3881/ab339a

    2019 doi

  27. [35]

    2001, in Astronomische Gesellschaft Meeting Abstracts, Vol

    Kroupa , P. 2001, in Astronomische Gesellschaft Meeting Abstracts, Vol. 18, Astronomische Gesellschaft Meeting Abstracts, P78

    2001

  28. [36]

    2007, in IAU Symposium, Vol

    Kun , M. 2007, in IAU Symposium, Vol. 237, Triggered Star Formation in a Turbulent ISM, ed. B. G. Elmegreen & J. Palous , 119--123

    2007

  29. [37]

    J., Mamajek , E

    Kun , M., Balog , Z., Kenyon , S. J., Mamajek , E. E., & Gutermuth , R. A. 2009, , 185, 451, 10.1088/0067-0049/185/2/451

    2009 doi

  30. [38]

    T., & Balog , Z

    Kun , M., Kiss , Z. T., & Balog , Z. 2008, in Handbook of Star Forming Regions, Volume I, ed. B. Reipurth , Vol. 4, 136

    2008

  31. [39]

    L., Valette , B., et al

    Lallement , R., Vergely , J. L., Valette , B., et al. 2014, , 561, A91, 10.1051/0004-6361/201322032

    2014 doi

  32. [40]

    2018, , 616, A132, 10.1051/0004-6361/201832832

    Lallement , R., Capitanio , L., Ruiz-Dern , L., et al. 2018, , 616, A132, 10.1051/0004-6361/201832832

    2018 doi

  33. [41]

    B., & Starrfield , S

    Larson , R. B., & Starrfield , S. 1971, , 13, 190

    1971

  34. [42]

    2020, , 901, 49, 10.3847/1538-4357/abaef3

    Li , L., Shao , Z., Li , Z.-Z., et al. 2020, , 901, 49, 10.3847/1538-4357/abaef3

    2020 doi

  35. [43]

    2019, , 245, 32, 10.3847/1538-4365/ab530a

    Liu , L., & Pang , X. 2019, , 245, 32, 10.3847/1538-4365/ab530a

    2019 doi

  36. [44]

    M., Pisano , D

    McClure-Griffiths , N. M., Pisano , D. J., Calabretta , M. R., et al. 2009, , 181, 398, 10.1088/0067-0049/181/2/398

    2009 doi

  37. [45]

    1987, , 317, 190, 10.1086/165267

    McCray , R., & Kafatos , M. 1987, , 317, 190, 10.1086/165267

    1987 doi

  38. [46]

    Miret-Roig , N., Galli , P. A. B., Olivares , J., et al. 2022, , 667, A163, 10.1051/0004-6361/202244709

    2022 doi

  39. [47]

    A., Meschin , P

    Olano , C. A., Meschin , P. I., & Niemela , V. S. 2006, , 369, 867, 10.1111/j.1365-2966.2006.10343.x

    2006

  40. [48]

    2022, , 931, 156, 10.3847/1538-4357/ac674e

    Pang , X., Tang , S.-Y., Li , Y., et al. 2022, , 931, 156, 10.3847/1538-4357/ac674e

    2022 doi

  41. [49]

    E., Alves , J., et al

    Ratzenb \"o ck , S., Gro schedl , J. E., Alves , J., et al. 2023, , 678, A71, 10.1051/0004-6361/202346901

    2023 doi

  42. [50]

    J., Menten , K

    Reid , M. J., Menten , K. M., Brunthaler , A., et al. 2019, , 885, 131, 10.3847/1538-4357/ab4a11

    2019 doi

  43. [51]

    2024, , 534, 2566, 10.1093/mnras/stae2157

    S \'a nchez-Sanju \'a n , S., Hern \'a ndez , J., P \'e rez-Villegas , \'A ., et al. 2024, , 534, 2566, 10.1093/mnras/stae2157

    2024 doi

  44. [52]

    Schinnerer , E., & Leroy , A. K. 2024, , 62, 369, 10.1146/annurev-astro-071221-052651

    2024 doi

  45. [53]

    2010, , 403, 1829, 10.1111/j.1365-2966.2010.16253.x

    Sch \"o nrich , R., Binney , J., & Dehnen , W. 2010, , 403, 1829, 10.1111/j.1365-2966.2010.16253.x

    2010

  46. [54]

    Spoelstra , T. A. T. 1973, , 24, 149

    1973

  47. [55]

    2021, , 505, 5164, 10.1093/mnras/stab1496

    Szil \'a gyi , M., Kun , M., & \'A brah \'a m , P. 2021, , 505, 5164, 10.1093/mnras/stab1496

    2021 doi

  48. [56]

    Taylor , M. B. 2005, in Astronomical Society of the Pacific Conference Series, Vol. 347, Astronomical Data Analysis Software and Systems XIV, ed. P. Shopbell , M. Britton , & R. Ebert , 29

    2005

  49. [57]

    2017, PhD thesis, University of Groningen

    Tian, H. 2017, PhD thesis, University of Groningen

    2017

  50. [58]

    C., & Varoquaux , G

    van der Walt , S., Colbert , S. C., & Varoquaux , G. 2011, Computing in Science and Engineering, 13, 22, 10.1109/MCSE.2011.37

    2011 doi

  51. [59]

    2025, , 979, 92, 10.3847/1538-4357/ad960a

    Wang , F., Fang , M., Fu , X., et al. 2025, , 979, 92, 10.3847/1538-4357/ad960a

    2025 doi

  52. [60]

    2016, , 585, A41, 10.1051/0004-6361/201527007

    Winkel , B., Kerp , J., Fl \"o er , L., et al. 2016, , 585, A41, 10.1051/0004-6361/201527007

    2016 doi

  53. [61]

    2022, Research in Astronomy and Astrophysics, 22, 085017, 10.1088/1674-4527/ac784e

    Xia , J., Tang , N., Zhi , Q., et al. 2022, Research in Astronomy and Astrophysics, 22, 085017, 10.1088/1674-4527/ac784e

    2022 doi

  54. [62]

    Zari , E., Brown , A. G. A., & de Zeeuw , P. T. 2019, , 628, A123, 10.1051/0004-6361/201935781

    2019 doi

  55. [63]

    J., Liu , Y., Fang , M., & Kuhn , M

    Zhou , X., Herczeg , G. J., Liu , Y., Fang , M., & Kuhn , M. 2022, , 933, 77, 10.3847/1538-4357/ac704d

    2022 doi

  56. [64]

    2024, , 966, 202, 10.3847/1538-4357/ad3552

    Zhuang , Z., Su , Y., Zhang , S., et al. 2024, , 966, 202, 10.3847/1538-4357/ad3552

    2024 doi

  57. [65]

    2023, in Astronomical Society of the Pacific Conference Series, Vol

    Zucker , C., Alves , J., Goodman , A., Meingast , S., & Galli , P. 2023, in Astronomical Society of the Pacific Conference Series, Vol. 534, Protostars and Planets VII, ed. S. Inutsuka , Y. Aikawa , T. Muto , K. Tomida , & M. Tamura , 43

    2023

Pith tools

Reviewed August 16, 2026 · model on record in the stance chip above.