Minute-Cadence Observations of the LAMOST Fields with the TMTS: IV—Catalog of Cataclysmic Variables from the First 3-yr Survey
, Jie Lin 1,2,3,*, Xiaofeng Wang 1,*, Zhibin Dai 4,5, Yongkang Sun 6,7, Gaobo Xi 1, Jun Mo 1, Jialian Liu 1, Shengyu Yan 1, Alexei V. Filippenko 8, Thomas G. Brink 8, Yi Yang 1,8, Kishore C. Patra 8, Yongzhi Cai 4,5,9, Zhihao Chen 1, Liyang Chen 1, Fangzhou Guo 1, Xiaojun Jiang 7,10,11, Gaici Li 1, Wenxiong Li 10, add
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Round 1
Reviewer 1 Report
Comments and Suggestions for AuthorsReferee report to the paper “Minute-cadence observations of the LAMOST fields with the TMTS: IV. Catalogue of cataclysmic variables from the first 3-yr survey” by Qichun Liu et al.
The authors presented the photometric observations of some cataclysmic variable stars
(CVs) performed with the Tsinghua University–Ma Huateng Telescopes for Survey (TMTS). They obtained one-night light curves of 57 CVs and seven candidates. Using these
light curves Qichun Liu with the co-authors tried to determine photometric
periods. Unfortunately, the accuracy of the obtained periods are very low because
it is hard to find accurate period if the duration of the observations are only in 3-4 times longer. Nevertheless, the paper could be published after minor revision because
a new light curves for a couple of CV candidates were obtained.
Remarks
1) Table 1, the column "VSX Name". There are 0 instead of space in the several CV names,
e.g. V0709 Cas instead of V 709 Cas.
2) Subsection 3.1.1. The CV was classified as a very long-duration quiescence CV.
But the spectrum shows the absorption Balmer lines (e.g. H_beta), which are rather
corresponds to a nova-like system with the optically thick accretion disc. Moreover,
the line He II 4686 does not evidence of nova-like systems, but the feature related
to magnetic CVs.
3) Subsection 3.2.1. The source was classified as a VY Scl system. But a relatively strong HeII 4686 line is typical for magnetic CVs. Moreover, a significant brightness variations is also typical for polars, not only for anti-dwarf novae.
4) Figure 5. The caption does not correspond to the panels.
5) Line 254 (Subsection 3.2.3.) There is a typo, Hff instead of H_alpha ?
6) The title of Sect. 4. Have to be "Discussion" instead of "discussion".
7) Page 17, the second paragraph (lines 368-372). The authors discussed the possibility that the brightness variation of FO Per is due to the reflection effect. It is not possibly, the luminosity of the white dwarf + the inner accretion disc is not enough for that. This paragraph has to be excluded.
Author Response
Please see the attachment.
Author Response File: 
Author Response.pdf
Reviewer 2 Report
Comments and Suggestions for Authors Dear authors,
I have following suggestions for correcting of your manuscript.
line 65:
correct "...improve ourunderstanding of..." to
"...improve our understanding of ..."
line 175:
The TESS abbreviation has already been explained on line 64.
So, here use just "TESS".
Figure 3:
- Please, clarify the y-label "Scaled flux" for the spectrum in
the top panel. How the spectrum is scaled ?
- Add the tics to the y2-axis.
line 254:
What is the "Hff" emission? Please, correct or clarify.
Table 2:
Please, clarify the meaning of the indices "mean" and "std"
in the caption of Table 2.
line 348:
I suggest to correct, "...and thus suffer an intenser Kepler
broadening. " to "...and thus suffer from a more intense Kepler
broadening. "
5. Conclusions:
I suggest using past tense.
The statement "We attempt to apply these features to explore
the fast-developing physical process in CVs, which help the CV
subclassification." is too general and vague. Try to be more
specific (if possible).
Author Response
Please see the attachment.
Author Response File: Author Response.pdf
