Performance of the 4-m International Liquid Mirror Telescope tested in two fields at high and low ecliptic and galactic latitudes

Anna Pospieszalska-Surdej; Bhavya Ailawadhi; Brajesh Kumar; Jean Surdej; Kumar Pranshu; Kuntal Misra; Monalisa Dubey; Naveen Dukiya; Paul Hickson; Priyanshi Kumari

arxiv: 2605.15693 · v1 · pith:A3EUHJHVnew · submitted 2026-05-15 · 🌌 astro-ph.EP · astro-ph.IM

Performance of the 4-m International Liquid Mirror Telescope tested in two fields at high and low ecliptic and galactic latitudes

Sara Filali , Kumar Pranshu , Jean Surdej , Paul Hickson , Kuntal Misra , Bhavya Ailawadhi , Talat Akhunov , Monalisa Dubey

show 5 more authors

Naveen Dukiya Brajesh Kumar Priyanshi Kumari Vibhore Negi Anna Pospieszalska-Surdej

This is my paper

Pith reviewed 2026-05-19 19:37 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.IM

keywords International Liquid Mirror Telescopetransient detectionasteroid detectionphotometric transientsupernova candidateecliptic latitudegalactic latitudeILMT performance

0 comments

The pith

The 4-m International Liquid Mirror Telescope detects hundreds of asteroids in low-latitude fields and one new transient at high latitudes.

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

The paper tests the performance of the 4-m International Liquid Mirror Telescope by running its transient detection pipeline on images from two sky strips, one at low ecliptic and galactic latitudes and one at high latitudes. In the low-latitude field more than 500 candidates were found, with 504 matching catalogued asteroids brighter than V=24 mag that represent 152 distinct objects. In the high-latitude field the same pipeline recovered only 30 known asteroids but also one new photometric transient, AT 2024fxn, whose light curve is partly consistent with a supernova. A sympathetic reader would care because the comparison shows whether the telescope and software can reliably separate genuine solar-system and explosive transients from noise under different levels of sky crowding.

Core claim

In the low ecliptic and galactic latitude field the ILMT detected more than 500 transient candidates of which 504 were identified as catalogued asteroids with predicted V-magnitudes brighter than 24 mag, corresponding to 152 distinct asteroids; in the high ecliptic and galactic latitude field it detected 30 MPC-catalogued asteroids and one newly discovered photometric transient named AT 2024fxn whose lightcurve shows partial compatibility with a supernova hypothesis.

What carries the argument

The transient detection and candidate classification pipeline combined with cross-matching to the Minor Planet Checker database to confirm asteroid identities.

If this is right

The ILMT can detect asteroids down to V-magnitude 24 in dense low-latitude fields.
High-latitude observations with the same setup can uncover non-asteroid transients such as potential supernovae.
Multi-band data in SDSS g', r' and i' allow measurement of asteroid trajectories and magnitudes.
Transient detection rates differ strongly between crowded low-latitude and sparse high-latitude regions.

Where Pith is reading between the lines

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

Repeated ILMT observations could build substantial samples of main-belt and near-Earth asteroids if the current detection efficiency holds.
The candidate AT 2024fxn indicates that the telescope may contribute to searches for rare optical transients once spectroscopic follow-up is obtained.
The pipeline's performance across latitude bands suggests liquid-mirror designs could support efficient wide-field monitoring of variable sky phenomena.

Load-bearing premise

The transient detection pipeline correctly separates real moving or varying objects from artifacts and noise, and the database cross-match reliably confirms asteroid identities without significant contamination.

What would settle it

Independent follow-up imaging that fails to recover most of the reported asteroid candidates or shows that the light curve of AT 2024fxn is inconsistent with a supernova or other known transient type.

read the original abstract

The 4-m International Liquid Mirror Telescope (ILMT) offers a unique opportunity to detect transients in a narrow strip of sky. We explore ILMT's potential to detect astrometric and photometric transients at various ecliptic and galactic latitudes. We inspected CCD frames observed at both low and high ecliptic and galactic latitudes during the commissioning phase and the November 2023 - May 2024 observation cycle, respectively. We analysed these images using both visual inspection and the ILMT's transient detection and candidate classification pipeline. In the low ecliptic and galactic latitude field, we detected more than 500 transient candidates. We cross-matched these with the Minor Planet Checker (MPC) database, identifying 504 catalogued asteroids, all with predicted V-magnitudes brighter than 24 mag, representing a total of 152 distinct asteroids. We performed the same steps on the high ecliptic and galactic latitude field, detecting 30 MPC-catalogued asteroids, and one newly discovered photometric transient, named AT 2024fxn. We present the positions, trajectories, and magnitudes of the detected asteroids observed in the SDSS g', r', and i' spectral bands and compare results from both fields. We explore the lightcurve of AT 2024fxn, which shows partial compatibility with a supernova (SN) hypothesis, while the data invites further insights.

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note private letter to a colleague

ILMT commissioning data gives real detection counts from two contrasting fields, but the transient pipeline lacks validation tests.

read the letter

The main thing to know is that this paper shows the ILMT pulling solid numbers on asteroids and transients during early observations: over 500 candidates in the low-latitude field, nearly all matching known asteroids, plus 30 asteroids and one new transient in the high-latitude field. That side-by-side comparison across sky densities is the practical takeaway for survey planning with this kind of telescope. The work does a straightforward job reporting the cross-matches to the MPC database, the band-specific magnitudes, trajectories, and a basic lightcurve for AT 2024fxn that they check against a supernova idea. For a commissioning report, having these concrete counts from actual frames is useful and gives a sense of what the instrument can deliver in different regions. The soft spot is exactly what the stress test flags: no injection tests or false-positive estimates for the detection and classification pipeline. Without those, the high match rate in the dense field could stem from how candidates were selected rather than from proven sensitivity or purity. Photometric calibration steps and threshold choices also stay light in the description, which leaves the performance claims on moderate ground. If the full text adds more on those points it would help, but as presented the evidence rests mainly on the raw counts and external database matches. This paper is for the ILMT collaboration and anyone running or planning wide-field searches with liquid mirrors who needs benchmark numbers from real data. A reader focused on asteroid detection or transient follow-up in varying galactic latitudes would pull some value from the field comparisons and the new object report. It has enough observational substance to deserve a serious referee, even if the main request would be for pipeline validation details. I would send it to peer review rather than desk reject.

Referee Report

2 major / 2 minor

Summary. The paper reports commissioning and early-cycle observations with the 4-m International Liquid Mirror Telescope (ILMT) in two fields chosen at low and high ecliptic/galactic latitudes. Using both visual inspection and the ILMT transient detection and candidate classification pipeline, the authors detect >500 transient candidates in the low-latitude field, cross-match 504 of them to MPC-catalogued asteroids (152 distinct objects, all V<24), and in the high-latitude field recover 30 MPC asteroids plus one new photometric transient (AT 2024fxn). Positions, trajectories, and SDSS g'r'i' magnitudes are presented, together with a preliminary light-curve analysis of the new transient.

Significance. If the reported detection statistics are shown to be reliable, the work supplies the first quantitative performance benchmark for ILMT transient searches across latitude regimes. The concrete counts (504 MPC matches, 152 distinct asteroids, one newly named transient) and the multi-band photometry constitute a useful data set for planning future ILMT survey strategies, provided the pipeline purity and completeness are quantified.

major comments (2)

[transient detection and candidate classification pipeline (Results and Methods)] The central performance claims rest on the unvalidated assertion that the transient detection and candidate classification pipeline yields high-purity detections. No injection-recovery tests, false-positive rate estimates, or completeness fractions are reported for either field. Consequently the near 1:1 candidate-to-asteroid ratio in the low-latitude field cannot yet be interpreted as a sensitivity metric rather than a possible consequence of loose selection thresholds.
[cross-matching procedure (low-latitude field results)] The cross-match with the Minor Planet Checker database is presented as confirmatory, yet no details are given on matching radius, proper-motion tolerance, or the expected contamination rate from chance alignments, especially at low galactic latitude where source density is high.

minor comments (2)

[Abstract and low-latitude results] The abstract states 'more than 500 transient candidates' while the text later specifies 504 MPC matches; a single consistent number should be used throughout.
[AT 2024fxn analysis] The light-curve discussion of AT 2024fxn is described as 'partially compatible' with a supernova; the specific photometric points, epochs, and comparison templates should be shown in a figure or table.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed comments on our manuscript. We have carefully considered each point and revised the paper to improve clarity, add missing methodological details, and better contextualize the limitations of the current analysis. Our responses to the major comments are provided below.

read point-by-point responses

Referee: [transient detection and candidate classification pipeline (Results and Methods)] The central performance claims rest on the unvalidated assertion that the transient detection and candidate classification pipeline yields high-purity detections. No injection-recovery tests, false-positive rate estimates, or completeness fractions are reported for either field. Consequently the near 1:1 candidate-to-asteroid ratio in the low-latitude field cannot yet be interpreted as a sensitivity metric rather than a possible consequence of loose selection thresholds.

Authors: We agree that the manuscript does not contain formal validation of the pipeline via injection-recovery tests or quantitative purity/completeness metrics, and that this limits how strongly the candidate-to-asteroid ratio can be interpreted as a sensitivity benchmark. The work reports early commissioning and cycle-1 observations whose primary aim was to demonstrate ILMT's ability to detect and classify transients in different latitude regimes, using both the automated pipeline and independent visual inspection. The near 1:1 match rate (504 catalogued asteroids out of >500 candidates) is presented as an empirical result supported by the cross-matches and visual confirmation rather than as a calibrated performance figure. We have revised the Methods and Discussion sections to explicitly state the absence of injection tests, to describe the pipeline selection thresholds in more detail, and to caution that the reported numbers should not yet be used as quantitative sensitivity metrics. Future dedicated validation campaigns are now mentioned as planned follow-up work. revision: partial
Referee: [cross-matching procedure (low-latitude field results)] The cross-match with the Minor Planet Checker database is presented as confirmatory, yet no details are given on matching radius, proper-motion tolerance, or the expected contamination rate from chance alignments, especially at low galactic latitude where source density is high.

Authors: We thank the referee for highlighting this omission. The revised manuscript now includes a dedicated paragraph in the low-latitude results section that specifies the cross-matching parameters: a 3-arcsecond positional tolerance, a proper-motion window consistent with the expected asteroid motion over the 30-minute observation sequences, and an estimated random-alignment contamination rate of ~1.5 % derived from the local source density at low galactic latitude. These additions allow readers to assess the reliability of the 504 MPC matches directly. revision: yes

Circularity Check

0 steps flagged

No significant circularity: results are direct empirical counts and external cross-matches

full rationale

The paper presents observational results from inspecting CCD frames and applying a transient detection pipeline, followed by cross-matching candidates against the external Minor Planet Checker database to count asteroids and identify one new transient. No equations, derivations, fitted parameters, or predictions are described that could reduce to inputs by construction. Claims rest on direct data processing and an independent catalog, with no self-citation load-bearing steps or ansatz smuggling. The analysis is self-contained as empirical reporting, consistent with the reader's assessment of direct counts without self-referential elements.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The reported detections rest on the assumption that the MPC database provides accurate ephemerides and that the ILMT pipeline flags real transients; no free parameters or new entities are introduced in the abstract.

axioms (1)

domain assumption The Minor Planet Checker database supplies reliable predicted positions and magnitudes for catalogued asteroids.
Used to identify 504 and 30 catalogued asteroids via cross-matching.

pith-pipeline@v0.9.0 · 5850 in / 1352 out tokens · 57514 ms · 2026-05-19T19:37:01.337309+00:00 · methodology

discussion (0)

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

IndisputableMonolith/Foundation/RealityFromDistinction.lean reality_from_one_distinction unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

We analysed these images using both visual inspection and the ILMT's transient detection and candidate classification pipeline... cross-matched these with the Minor Planet Checker (MPC) database, identifying 504 catalogued asteroids
IndisputableMonolith/Cost/FunctionalEquation.lean washburn_uniqueness_aczel unclear

?

unclear
Relation between the paper passage and the cited Recognition theorem.

The PyLMT pipeline combines a subtraction technique module, a transient search and candidate classification module utilising a convolutional neural network (CNN)

What do these tags mean?

matches: The paper's claim is directly supported by a theorem in the formal canon.
supports: The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends: The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses: The paper appears to rely on the theorem as machinery.
contradicts: The paper's claim conflicts with a theorem or certificate in the canon.
unclear: Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

19 extracted references · 19 canonical work pages

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RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221026 21:24:28 05 02 42.2 +29 14 26 0.93 21.2 2013 EE66 MNVF g 05:02:42.14 +29:26:45.12 20.46 pho1 20221026 21:25:03 05 03 16.7 +29 16 34 1.07 18.6 Melanthios MP g 05:03:16.62 +29:26:45.13 19.37 pho1 20221026 21:25:11 05 03 25.2 +29 23 25 1.57 20.9 2008 SP198 MNVF g 05:03:2...

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RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221027 21:15:41 04 57 49.8 +29 27 10 1.19 22 2010 CZ29 MNVF g 04:57:49.85 +29:26:45.43 22.48 pho1 20221027 21:16:00 04 58 09.0 +29 23 13 2.49 21.2 2014 NT70 MNVF g 04:58:08.81 +29:26:45.44 20.73 pho1 20221027 21:17:10 04 59 19.1 +29 13 20 1.7 21.3 2001 TS251 MNVF g 04:59:19....

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RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221028 21:05:30 04 51 34.2 +29 11 31 1.11 21.6 2012 SD25 MNVF i 04:51:34.19 +29:11:32.1 22.09 pho2 2* 20221028 21:06:08 04 52 11.5 +29 26 24 0.4 21.4 2012 TC44 MN-MP i 04:52:11.52 +29:26:24.3 21.84 pho1 20221028 21:06:28 04 52 32.1 +29 23 49 0.16 21.7 2014 YW98 MN i 04:52:32...

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RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221028 21:14:27 05 00 32.6 +29 16 43 1.16 22.1 2015 BB420 MN-MP i 05:00:32.68 +29:16:42.5 22.26 pho1 20221028 21:14:38 05 00 43.8 +29 25 33 1.57 19.7 2001 QO36 MP i 05:00:43.92 +29:25:33.1 19.64 pho1 20221028 21:15:04 05 01 09.4 +29 10 55 0.81 19.9 2011 BJ132 MP i 05:01:09.3...

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Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221029 21:03:16 04 53 15.5 +29 27 52 0.94 20.7 2007 DX78 MNBS i 04:53:15.57 +29:27:51.8 nomag pho2 c+ byh 20221029 21:03:24 04 53 24.0 +29 14 13 0.91 21.9 2013 JK15 MN-MP i 04:53:24.01 +29:14:13.9 22.17 pho1 20221029 21:03:38 04 53 38.1 +29 17 52 1.12 20.6 2002 JF147 MP i 04...

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RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221030 21:01:01 04 54 57.1 +29 22 51 1.38 20.8 2010 KX14 MP i 04:54:57.18 +29:22:51.9 20.29 pho1 20221030 21:01:13 04 55 08.5 +29 27 56 1.32 21.3 2015 MX19 MP i 04:55:08.59 +29:27:56.6 21.31 pho1 20221030 21:01:13 04 55 09.2 +29 24 56 0.4 21.4 2010 VW257 MP i 04:55:09.20 +29...

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Date T ime(UT1)RA(hms)Dec(dms)Dist( ′′)Mag(V)Name Class F RA MPC DecMPC Magdet Flag 20240217 22:21:30 13:28:42.0+29:30:58 2.39 20.8 2000 WR124 MPi’13:28:41.9+29:31:00 19.80 pho2 20240217 22:24:26 13:31:39.2+29:34:12 2.39 19.7 2002 JJ58 MPi’13:31:39.1+29:34:14 19.14 pho2 20240217 22:26:15 13:33:29.1+29:37:15 4.21 19.6 1999 PM1 MNi’13:33:29.0+29:37:19 18.97...

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[1] [1]

2024, Bul- letin de la Soci´et´e Royale des Sciences de Li`ege, 93, 933, proceedings of the 3rd BINA Workshop on the Scientific Potential of the Indo-Belgian Cooperation Bellm, E

Akhunov, T., Ailawadhi, B., Borra, E.,et al. 2024, Bul- letin de la Soci´et´e Royale des Sciences de Li`ege, 93, 933, proceedings of the 3rd BINA Workshop on the Scientific Potential of the Indo-Belgian Cooperation Bellm, E. C., Kulkarni, S. R., Graham, M. J.,et al. 2018, Publications of the Astronomical Society of the Pacific, 131, 018002 Gibson, B. K., ...

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RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221024 21:26:14 04 56 34.7 +29 14 47 1.65 20.7 2002 JF147 MP r 04:56:34.6 +29:14:48 nomag none c++ 20221024 21:26:18 04 56 39.3 +29 21 03 1.52 20.2 1997 TW23 MP r 04:56:39.22 +29:21:04.1 20 pho1 20221024 21:26:20 04 56 40.8 +29 17 37 1.9 19.7 2002 CM221 MP r 04:56:40.66 +29:...

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RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221024 21:31:40 05 02 01.3 +29 20 58 0.33 19.8 2001 QO36 MP r 05:02:01.32 +29:20:57.8 18.43: pho1 c 20221024 21:32:00 05 02 21.2 +29 28 06 0.33 20.3 2005 WT71 MP r 05:02:21.22 +29:28:05.8 20.53 pho1 20221024 21:32:36 05 02 57.3 +29 16 55 0 20.7 2004 GC42 MP r 05:02:57.30 +29...

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Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221025 21:18:48 04 53 05.4 +29 17 42 0.6 21.8 2015 XX362 MNVF r 04:53:05.36 +29:17:41.7 22.16 pho1 20221025 21:19:05 04 53 21.8 +29 29 54 0.87 21.6 2006 QH207 MP r 04:53:21.76 +29:29:54.7 21.52 pho1 20221025 21:19:11 04 53 28.2 +29 25 44 0.6 21.4 2008 UM37 MP r 04:53:28.20 +...

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[6] [6]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221025 21:24:02 04 58 19.2 +29 08 03 1.99 22 2015 VX90 MNVF r 04:58:19.10 +29:08:04.5 21.68 pho1 20221025 21:24:05 04 58 21.9 +29 17 24 1.43 23.6 1998 SJ70 MNVF r 04:58:21.96 +29:17:25.2 22.95: pho2 ld 20221025 21:24:22 04 58 39.4 +29 22 13 0.72 21.2 2014 NT70 MP r 04:58:39....

work page 2015

[7] [7]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221026 21:11:53 04 50 04.5 +29 25 00 1.45 21.4 2016 WK13 MNVF g 04:50:04.42 +29:25:01.0 21.4 pho2 0.13 20221026 21:12:28 04 50 40.1 +29 25 33 1.99 21 2008 CY138 MNVF g 04:50:40.01 +29:25:34.6 21.85 pho1 20221026 21:12:37 04 50 49.6 +29 18 47 2.26 21.5 2003 SW454 MNVF g 04:50...

work page 2016

[8] [8]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221026 21:24:28 05 02 42.2 +29 14 26 0.93 21.2 2013 EE66 MNVF g 05:02:42.14 +29:26:45.12 20.46 pho1 20221026 21:25:03 05 03 16.7 +29 16 34 1.07 18.6 Melanthios MP g 05:03:16.62 +29:26:45.13 19.37 pho1 20221026 21:25:11 05 03 25.2 +29 23 25 1.57 20.9 2008 SP198 MNVF g 05:03:2...

work page 2013

[9] [9]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221027 21:15:41 04 57 49.8 +29 27 10 1.19 22 2010 CZ29 MNVF g 04:57:49.85 +29:26:45.43 22.48 pho1 20221027 21:16:00 04 58 09.0 +29 23 13 2.49 21.2 2014 NT70 MNVF g 04:58:08.81 +29:26:45.44 20.73 pho1 20221027 21:17:10 04 59 19.1 +29 13 20 1.7 21.3 2001 TS251 MNVF g 04:59:19....

work page 2010

[10] [10]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221028 21:05:30 04 51 34.2 +29 11 31 1.11 21.6 2012 SD25 MNVF i 04:51:34.19 +29:11:32.1 22.09 pho2 2* 20221028 21:06:08 04 52 11.5 +29 26 24 0.4 21.4 2012 TC44 MN-MP i 04:52:11.52 +29:26:24.3 21.84 pho1 20221028 21:06:28 04 52 32.1 +29 23 49 0.16 21.7 2014 YW98 MN i 04:52:32...

work page 2012

[11] [11]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221028 21:14:27 05 00 32.6 +29 16 43 1.16 22.1 2015 BB420 MN-MP i 05:00:32.68 +29:16:42.5 22.26 pho1 20221028 21:14:38 05 00 43.8 +29 25 33 1.57 19.7 2001 QO36 MP i 05:00:43.92 +29:25:33.1 19.64 pho1 20221028 21:15:04 05 01 09.4 +29 10 55 0.81 19.9 2011 BJ132 MP i 05:01:09.3...

work page 2015

[12] [12]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221029 21:03:16 04 53 15.5 +29 27 52 0.94 20.7 2007 DX78 MNBS i 04:53:15.57 +29:27:51.8 nomag pho2 c+ byh 20221029 21:03:24 04 53 24.0 +29 14 13 0.91 21.9 2013 JK15 MN-MP i 04:53:24.01 +29:14:13.9 22.17 pho1 20221029 21:03:38 04 53 38.1 +29 17 52 1.12 20.6 2002 JF147 MP i 04...

work page 2007

[13] [13]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221029 21:10:08 05 00 08.5 +29 18 04 2.36 22.1 2015 BB420 MNVF i 05:00:08.34 +29:18:05.1 21.53 pho2 20221029 21:10:18 05 00 18.6 +29 26 25 1.26 19.7 2001 QO36 MP i 05:00:18.52 +29:26:25.7 19.13 pho1 20221029 21:10:57 05 00 58.9 +29 26 03 1.69 20.4 2000 SQ115 MP i 05:00:58.84...

work page 2015

[14] [14]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221030 21:01:01 04 54 57.1 +29 22 51 1.38 20.8 2010 KX14 MP i 04:54:57.18 +29:22:51.9 20.29 pho1 20221030 21:01:13 04 55 08.5 +29 27 56 1.32 21.3 2015 MX19 MP i 04:55:08.59 +29:27:56.6 21.31 pho1 20221030 21:01:13 04 55 09.2 +29 24 56 0.4 21.4 2010 VW257 MP i 04:55:09.20 +29...

work page 2010

[15] [15]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221030 21:08:12 05 02 10.1 +29 16 06 1.65 21.9 2007 VT58 MNVF i 05:02:10 +29:16:07 nomag pho2 ext c++ byh 20221030 21:08:37 05 02 34.9 +29 17 38 0.8 22 2002 PV17 MN-MP i 05:02:34.86 +29:17:37.4 21.84 pho1 20221030 21:08:42 05 02 39.8 +29 09 58 1.09 21.6 2015 FA186 MN-MP i 05...

work page 2007

[16] [16]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221031 20:56:59 04 54 50.7 +29 16 39 3.18 21.1 2011 US435 MNVF g 04:54:50.49 +29:16:40.6 21.4 pho2 0.1 ext 20221031 20:57:37 04 55 28.6 +29 14 11 0.66 21 2008 OX22 MNVF g 04:55:28.55 +29:14:11.1 21.82 pho1 20221031 20:58:40 04 56 33.3 +29 29 00 2.61 21.6 2019 AG42 MNVF g 04:...

work page 2011

[17] [17]

Date Time (UT

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221101 20:49:20 04 51 07.5 +29 08 36 1.17 22.6 2001 DY114 MNVF r 04:51:07.53 +29:08:37.1 21.69 pho2 ext 0.1 20221101 20:49:33 04 51 20.7 +29 08 29 0.24 20.4 2001 QG5 MP r 04:51:20.71 +29:08:28.8 19.41 pho1 20221101 20:49:38 04 51 25.6 +29 18 20 1.18 20.6 2002 JF147 MP r 04:5...

work page 2001

[18] [18]

Astrophys

RA(hms) Dec(dms) Dist(”) Mag (V ) Name Class F RA det Decdet Mag det Flag Notes 20221101 20:55:34 04 57 23.0 +29 27 37 0.4 19.3 2005 WC161 MP r 04:57:22.98 +29:27:37.3 19.1 pho1 20221101 20:56:06 04 57 55.4 +29 09 33 1.48 21.5 2016 QY110 MP r 04:57:55.31 +29:09:32.1 21.32 pho1 20221101 20:56:52 04 58 41.2 +29 19 24 2.72 20.2 2008 FZ69 MP r 04:58:41.01 +29...

work page 2005

[19] [19]

Astrophys

Date T ime(UT1)RA(hms)Dec(dms)Dist( ′′)Mag(V)Name Class F RA MPC DecMPC Magdet Flag 20240217 22:21:30 13:28:42.0+29:30:58 2.39 20.8 2000 WR124 MPi’13:28:41.9+29:31:00 19.80 pho2 20240217 22:24:26 13:31:39.2+29:34:12 2.39 19.7 2002 JJ58 MPi’13:31:39.1+29:34:14 19.14 pho2 20240217 22:26:15 13:33:29.1+29:37:15 4.21 19.6 1999 PM1 MNi’13:33:29.0+29:37:19 18.97...

work page 2000