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4Peremennye Zvezdy ( Variable Stars) 43, No. 7, 2023 Received 28 August; accepted 10 September.
DOI: 10.24412/2221-0474-43-55-85
Catalog of Multi-Mode Radially Pulsating Variables: I
A. V. Khruslov1'2
1 Sternberg Astronomical Institute, Moscow State University, Universitetskij pr. 13, Moscow 119992, Russia; khruslov@bk.ru
2 Institute of Astronomy, Russian Academy of Sciences, Pyatnitskaya str. 48, Moscow 119017, Russia
I present a catalog of newly detected Multi-Mode Radially Pulsating (MMRP) variable stars that pulsate in the fundamental, first, second, or third-overtone modes. This catalog includes 50 double- and multi-mode stars. Among variability types of these stars, we find classical Cepheids, RR Lyrae, and high-amplitude S Scuti (HADS) variables. Additionally, I studied 14 known multi-periodic variables.
I analyzed all observations available for these stars in the ASAS-SN and ZTF online public archives using the period-search software developed by Dr. V.P. Goranskij for Windows environment. Light elements and parameters of oscillations were determined.
1 Introduction
In the course of my search for double-mode and multiperiodic variable stars using available photometric archives, I detected 50 new Multi-Mode Radially Pulsating (MMRP) variables. These stars pulsate in the fundamental, first-overtone, second-overtone, or third-overtone modes. This article continued the series of my previous papers (Khruslov. 2018a, 2021a, 2022, etc.). Among variability types of these stars, we find classical Cepheids, RR Lyrae stars, and high-amplitude 8 Scuti variables.
Additionally, I studied 14 known multi-periodic variables (see additional Tables with index 'a') as a part of the program of preparation for their inclusion in the General Catalog of Variable Stars, GCVS (Samus et al., 2017).
Searching for double periodicity, I mainly used data available in the photometric archive of the All-Sky Automated Survey for Supernovae (ASAS-SN, Shappee et al., 2014; Kochanek et al., 2017) and the Zwicky Transient Facility (ZTF, Bellm et al., 2019; Masci et al., 2019)
The method I use to search for multiperiodicity is similar to that described in my earlier paper (Khruslov, 2021). To search for candidate multi-mode variables, I used AAVSO VSX1 database, the ASAS-SN catalogs of variable stars2 database (Jayasinghe et al., 2018, 2019a, 2019b, 2020, 2021), ZTF catalog of periodic variable stars3, Chen et al. (2020).
The radial pulsation modes were identified by their period ratio (Pshort/Plong); see the study on this problem by Petersen (1973), Petersen & Christensen-Dalsgaard (1996), Smolec & Moskalik (2010), and others.
1 http://www.aavso.org/vsx/index.php?view=search.top
2 https://asas-sn.osu.edu/variables
3 http://variables.cn:88/ztf/
2 Photometric data
For this study, I used the data of the ASAS-SN4 database and the ZTF data available through the SNAD ZTF viewer5, Malanchev et al. (2021). The light elements are based on data from these two surveys, individual cases are described in Comments. The magnitude ranges and amplitudes in the tables are given according to this data. I used V and g bands of ASAS-SN, and r and g bands of ZTF.
Additionally, in individual cases, I analyzed available data from other archives: the Wide Angle Search for Planets (SuperWASP6, Butters et al., 2010; 8 variables), the Catalina Sky Surveys (CSS7, Drake et al., 2009; 5 variable), the All Sky Automated Survey (ASAS-38, Pojmanski 2002; 2 variables).
The ASAS-3 data used in this paper were downloaded before April 2022, in accordance to requirements of authors of this survey for users located in Russia.
The SuperWASP observations are available as FITS tables, which were converted into ASCII tables using the OMC2ASCII9 program, as described by Sokolovsky (2007).
The survey data used in this study for the program stars are available online in the html version of this paper as a zip archive. This file also includes all light curves of the variables and cross-identification tables for all stars.
In individual cases, the ZTF data contained continuous data series with duration of a whole night of observations. This created some difficulties in the analysis of data. To eliminate these problems, we used averaged values (the mean for about 10 neighboring points) for our analysis. These averaged values are presented in the data files below the main data series. The rows of these supplements contain mean HJD times, mean magnitudes, and number of averaged points.
3 Identification names
In this paper, the following identification names are used for variables.
For new multi-periodic stars, with multi-periodicity first detected in this study, I use designations of the form MMRP-XXX (where MMRP is the name of the present program, aimed at discoveries of Multi-Mode Radially Pulsating variables, and XXX is the sequence number in the catalog). An example: MMRP-010.
For the known multi-periodic stars, for which this paper presents new light elements, I used designations in the form MMRPJXXXXXX.XX+XXXXXX.X (the abbreviation MMRP followed with equatorial coordinates for the equinox 2000.0). An example: MMRPJ054223.13+275647.6.
4 Classification
In the present paper, I use an original notation for types of multiperiodic variables. The basics of the classification were presented by N.N. Samus and the GCVS team at the XXVIIAU General Assembly in Prague, 200610: classical GCVS types of radial pulsating variables were appended with numbers of pulsation modes (0 - fundamental mode, 1 -
4 https://asas-sn.osu.edu/
5 https://ztf.snad.space/
6 http://wasp.cerit-sc.cz/form/
7 http://nunuku.caltech.edu/cgi-bin/getcssconedb_release_img.cgi
8 http://www.astrouw.edu.pl/asas/?page=aasc
9 http://scan.sai.msu.ru/swasp_converter/
10 http://www.sai.msu.su/gcvs/future/classif.htm
first overtone, 2 - second overtone). Double-mode variables are marked with a set of detected modes. For example, RR Lyrae stars can be designated as RR0, RR1, and RRB01 (in the old system, RRAB, RRC, and RR(B), respectively, B meaning "beat"). A similar notation was proposed for classical Cepheids (DCepO, DCepl, DCepB01, and DCepB12).
In the new MMRP classification, the numerical identification of pulsation modes is preserved, and the variability type is designated with a single letter. Additional characteristics are introduced with an additional index. An arrow indicates the cases of mode switching.
I. Types of variable stars:
C - classical Cepheids;
W - W Virginis, or type II Cepheids;
R - RR Lyrae stars;
D - ô Scuti stars.
II. Numbers of pulsation modes:
0 - fundamental mode;
1 - first overtone;
2 - second overtone;
3 - third overtone.
III. Addition designations:
n - additional non-radial mode;
m - amplitude modulation;
^ - mode switching.
Examples of designations of multi-periodic variables: C01, C12, C12m, D01, D123, D23, D12n, D0123, R01, W01, C12^C1, R01^R0, R1^R01.
The classical GCVS designations of mono-periodic variability types can be converted as follows: DCEP = C0, DCEPS = C1, RRAB = R0, RRC = R1; for multi-mode variable types, RR(b) type can be written as R01 (there are no R12 stars confirmed with certainty); CEP(B) is a group of types designated as C01, C12, C012, C123, and W01; DSCT(B) and SXPHE(B) is a group of all multi-mode D types.
The types from the VSX database are converted as follows: RRd = R01; DCEP(B) = C01; DCEPS(B) = C12; CWB(B) = W01; HADS(B) is a group of all multi-mode D types.
Double-mode type II Cepheids (W Virginis type) and mode-switching stars are not included in this catalog. An example of a W01 star, USN0-B1.0 0992-0344981, can be found in Khruslov (2021). An example of an R01^R0 star is USN0-B1.0 1171-0309158, see Khruslov et al. (2017). Other stars of these types may be included in later issues of MMPR catalogs.
in addition to type C12, I used type C*12 that includes stars morphologically close to type C12 but with shorter periods characteristic of R1 stars (see Subsection 6.3).
Besides the basic classification, I used two other indices: n for cases of detected additional non-radial modes; m for detected amplitude modulation with slow variation from
one season to another.
5 Results
5.1 Tables
For a correct presentation of information on multi-periodic variables in the MMRP catalog Tables, I use a multi-row format, with data presented in several sub-rows, each of them corresponding to an individual detected radial pulsation mode. Modes of pulsations are arranged in order of increasing pulsation frequency: the top sub-row is fundamental mode, the first overtone is below it, still lower are the second overtone, third overtone, and so on.
Each multi-row of the main Table (see Tables 1 and 1a) contains general information on the star: number in the Catalog of Multi-Mode Radially Pulsating (MMRS) stars; equatorial coordinates J2000 (for the earlier known MMRP stars, the coordinates are a part of the name); magnitude range (magnitudes at maximum and at minimum); type of multi-periodicity; and then, information about individual modes is presented in sub-rows (light elements, period and epoch of maximum; semi-amplitude; asymmetry parameter of the phased light curve, M-m). The period ratio (shorter period / longer period) is given for each pair of adjacent sub-rows (in the sub-row for the longer period).
The equatorial coordinates are given according to the Gaia EDR3 catalog. The tabulated magnitude range is for the photometric band indicated in brackets (aV and ag are ASAS-SN V and g magnitudes; zr and zg are ZTF r and g magnitudes). The data in these two columns are in two adjacent sub-rows. Coordinates: top - Right Ascension, bottom - Declination; magnitude range: top - maximum, bottom - minimum.
Individual mode characteristics: period is expressed in days; epoch is in one of the following formats: E = aX.XXXX = HJD — 2457777.0 or E = bX.XXXX = HJD — 2458888.0; semi-amplitude in the photometric band indicated in the "Magn." column; the M-m parameter is expressed in fractions of the period.
Tables 2 and 2a contain references to comments that supplement the data in the main table, and also provide information about the history of the variability studies for individual stars. The numbers correspond to the list below the tables.
Tables that supplement the main Table (Table 1 with Comments) follow, they contain general information on the stars. Tables 3 and 3a contain semi-amplitudes and magnitude ranges in all bands used in the ASAS-SN and ZTF surveys: aV, ag, zr, and zg. The data in "Magnitude range" columns is separated between two adjacent sub-rows: top - maximum, bottom - minimum. These tables contains amplitudes for four bands, so they partially duplicate Tables 1 and 1a. Tables 4 and 4a contain the known information according to catalogs and photometric surveys: color indices J — K (2MASS), B — V and g' — r' (APASS), g — V (ASAS-SN), and g — r (ZTF); and Galactic latitude (in degrees). These data are used for classification of variables.
Table 1. New Ml MRP variables
MMRP J2000 Magn. Type Period Epoch Ampl. M-m Ps/PL
001 00 02 40.26 +62 48 07.1 17.12 17.63 z9) D12m 0.221546 0.177851 b0.020 b0.150 0.159 0.060 0.40 0.50 0.8028
002 00 14 03.41 +61 51 26.8 15.40 15.94 zg) D123 0.2402248 0.1917915 0.1599293 b0.2335 b0.1130 b0.0683 0.149 0.034 0.039 0.44 0.47 0.45 0.7984 0.8339
003 00 53 46.41 + 16 30 17.6 17.73 18.47 zg) R01 0.553765 0.413406 b0.060 b0.345 0.086 0.224 0.44 0.34 0.7465
004 01 04 59.14 +63 11 37.9 16.12 16.70 zg) C12 0.517962 0.415517 b0.234 b0.282 0.230 0.018 0.50 0.48 0.8022
005 01 22 26.27 +59 12 36.2 12.26 12.68 ag) C*12 0.419811 0.335806 b0.347 b0.069 0.140 0.035 0.50 0.46 0.7999
006 01 41 37.16 +49 06 30.3 17.66 18.41 zg) R01 0.547006 0.408560 b0.148 b0.132 0.059 0.238 0.44 0.35 0.7469
007 02 35 16.88 +45 29 06.0 13.94 14.32 zg) D12 0.1171010 0.0955676 a0.0560 a0.0013 0.118 0.036 0.38 0.46 0.8161
008 03 28 13.47 +61 04 11.4 15.16 15.58 zr) C12 0.76234 0.61488 b0.703 b0.585 0.133 0.045 0.45 0.45 0.8066
009 04 50 39.61 +44 56 33.7 14.44 15.11 zg) C12 0.481392 0.385787 a0.122 a0.128 0.257 0.043 0.49 0.48 0.8014
010 04 53 16.75 +39 14 18.2 14.3715.21 ag) D0123 0.323070 0.243812 0.195780 0.163560 b0.036 b0.100 b0.113 b0.147 0.164 0.136 0.025 0.023 0.37 0.55 0.43 0.50: 0.7547 0.8030 0.8354
011 05 55 38.69 +27 03 19.9 13.99 14.48 zg) C*12 0.372014 0.298223 b0.039 b0.185 0.193 0.022 0.52 0.50 0.8016
012 06 32 45.23 -57 48 19.8 12.56 13.04 aV) D012 0.1202966 0.0910362 0.0732255 a0.1160 a0.0660 a0.0314 0.005 0.187 0.013 0.47 0.36 0.45 0.7568 0.8044
013 06 35 07.25 -02 24 39.4 18.12 18.81 zr) R01 0.485603 0.361474 b0.415 b0.370 0.127 0.155 0.44 0.38 0.7444
014 07 04 53.11 +72 56 03.8 16.53 17.61 zg) D012 0.0990373 0.0774669 0.0625011 b0.0412 b0.0343 b0.0240 0.208 0.111 0.036 0.33 0.41 0.43 0.7822 0.8068
Table 1 (continued)
MMRP J2000 Magn. Type Period Epoch Ampl. M-m Ps/PL
015 07 17 06.72 +02 10 06.3 14.11 14.50 z9) D12 0.1777760 0.1426887 b0.1080 b0.1100 0.128 0.032 0.45 0.48 0.8026
016 07 19 18.34 -57 21 50.8 14.01 14.50 aV) D12m 0.09090585 0.07264440 a0.0800 a0.0595 0.164 0.032 0.41 0.45 0.7991
017 07 34 28.23 -09 23 48.5 16.36 17.09 zg) R01 0.517177 0.385962 b0.253 b0.225 0.069 0.231 0.46 0.36 0.7463
018 07 41 56.58 -05 35 59.7 13.68 14.10 ag) D12 0.1170699 0.0937507 a0.0088 a0.0044 0.141 0.027 0.48 0.46 0.8008
019 07 42 26.28 -48 26 25.9 12.66 12.90 aV) D12m 0.1633818 0.1303208 b0.1555 b0.1240 0.080 0.007 0.54 0.48 0.7976
020 08 09 53.53 -24 00 01.5 12.66 13.16 ag) D23 0.1894973 0.1569780 b0.063 b0.095 0.174 0.034 0.30 0.48 0.8284
021 09 20 33.29 -53 23 17.3 13.24 13.57 ag) C12 0.962282 0.773766 b0.550 b0.567 0.100 0.026 0.44 0.50: 0.8041
022 10 14 19.37 -45 08 07.4 14.74 15.38 ag) D01n 0.1849927 0.1413880 b0.0420 b0.0640 0.113 0.108 0.38 0.55 0.7643
023 10 17 57.49 -43 33 27.5 12.99 13.30 ag) D12 0.1604404 0.1271510 b0.1380 b0.0520 0.106 0.013 0.53 0.46 0.7925
024 10 20 35.06 -45 27 09.0 13.50 14.03 ag) D012m 0.1828460 0.1401066 0.1120996 b0.1275 b0.0290 b0.1050 0.103 0.105 0.011 0.40 0.59 0.50 0.7663 0.8001
025 11 00 35.99 -00 33 15.9 17.95 18.50 zg) D01 0.0762403 0.0592999 b0.0522 b0.0572 0.134 0.057 0.39 0.49 0.7778
026 12 18 49.01 -40 36 23.7 13.73 14.11 ag) D12 0.1206566 0.0965767 a0.0237 a0.0860 0.132 0.012 0.56 0.47 0.8004
027 14 00 12.79 -57 59 22.8 11.46 11.75 ag) C*12 0.3422644 0.2735650 b0.886 b0.876 0.086 0.021 0.47 0.46 0.7993
028 15 23 19.83 -29 23 55.8 15.52 16.25 ag) D01 0.06193270 0.04790184 b0.0094 b0.0090 0.184 0.044 0.40 0.48 0.7734
029 16 36 55.57 -29 40 06.6 14.12 14.50 ag) D01 0.0961730 0.0742609 b0.0150 b0.0387 0.068 0.044 0.43 0.45 0.7722
Table 1 (continued)
ID J2000 Magn. Type Period Epoch Ampl. M-m Ps/PL
030 16 40 26.77 +02 17 42.7 14.76 15.34 ag) D01 0.06017101 0.04669287 b0.0103 b0.0006 0.132 0.069 0.40 0.44 0.7760
031 17 22 56.98 -37 09 12.4 14.29 14.78 ag) D23 0.1900259 0.1573530 a0.0420 a0.0870 0.143 0.032 0.44 0.46 0.8281
032 17 32 05.89 -29 55 58.7 13.15 13.48 aV) D12m 0.2959543 0.2361465 a0.0820 a0.0824 0.103 0.022 0.56 0.45 0.7979
033 18 04 41.13 -28 56 05.0 11.49 12.12 aV) D01m 0.1929179 0.1481671 a0.0292 a0.1310 0.199 0.056 0.37 0.47 0.7680
034 18 29 59.91 + 11 23 01.2 13.85 14.25 zg) D01 0.06896850 0.05332345 b0.1162 b0.0420 0.119 0.040 0.44 0.47 0.7732
035 18 39 23.75 -53 36 50.9 14.99 15.86 ag) D01 0.06268663 0.04906305 b0.0218 b0.0077 0.203 0.076 0.40 0.44 0.7827
036 19 13 05.48 + 12 38 02.2 14.97 15.66 zg) C01 5.6242 3.9115 b1.36 b0.49 0.195 0.104 0.42 0.49 0.6955
037 19 15 27.55 +09 06 01.1 14.93 15.28 zg) D12 0.1738900 0.1390354 b0.0180 b0.0206 0.086 0.060 0.48 0.47 0.7996
038 19 22 51.22 -59 07 05.4 14.40 14.72 ag) D12 0.06644163 0.05312860 b0.0434 b0.0421 0.071 0.032 0.46 0.45 0.7996
039 19 24 06.38 +26 48 08.3 14.72 15.24 zg) D012 0.1962641 0.1499660 0.1201920 b0.057 b0.063 b0.023 0.070 0.129 0.015 0.42 0.47 0.50 0.7641 0.8015
040 19 28 33.27 +23 29 20.2 14.87 15.37 zg) C*12 0.345059 0.275878 b0.134 b0.047 0.178 0.024 0.50 0.47 0.7995
041 19 40 49.14 +27 36 13.3 15.50 16.01 zg) D23 0.1608697 0.1327699 b0.0444 b0.0740 0.153 0.045 0.35 0.45 0.8253
042 19 44 01.74 +38 14 01.0 11.89 12.34 ag) C*12 0.335738 0.268255 a0.268 a0.102 0.161 0.026 0.50 0.47 0.7990
043 19 59 00.10 +29 28 26.3 17.26 18.06 zr) C01 0.840380 0.617996 b0.410 b0.460 0.127 0.117 0.34 0.40 0.7354
044 20 02 56.86 +23 20 32.1 11.73 12.05 ag) D12 0.1769232 0.1405731 b0.1637 b0.0410 0.104 0.021 0.44 0.45 0.7945
Table 1 (continued)
MMRP J2000 Magn. Type Period Epoch Ampl. M-m Ps/PL
045 20 05 50.64 +30 58 57.3 12.73 13.02 D23 0.09904520 0.08253105 b0.0340 b0.0415 0.089 0.029 0.43 0.47 0.8333
046 20 08 29.64 +30 59 48.9 18.16 18.64 (zr) C12 0.662711 0.530568 b0.470 b0.175 0.147 0.022 0.42 0.46 0.8006
047 20 35 44.04 +47 50 35.7 17.60 18.09 (zr) C12 0.702280 0.566057 b0.009 b0.473 0.151 0.033 0.47 0.44 0.8060
048 20 57 52.03 +49 27 23.5 17.80 18.20 (zr) C12 0.533432 0.427953 b0.235 b0.046 0.135 0.031 0.47 0.45 0.8023
049 22 38 26.91 +43 52 49.4 13.96 14.43 (zg) D01 0.1794143 0.1375285 a0.1080 a0.1310 0.047 0.156 0.45 0.57 0.7665
050 23 47 49.26 +64 21 47.4 16.55 17.34 (zg) C12 0.85364 0.68721 b0.470 b0.568 0.227 0.058 0.39 0.44 0.8050
Table 1a. Known multi-mode variables
MMRPJ Magn. Type Period Epoch Ampl. M-m Ps/PL
044322.93+465703.6 14.75 15.58 z9) C12 0.975593 0.782620 b0.165 b0.754 0.261 0.062 0.34 0.50 0.8022
054223.13+275647.6 12.89 13.61 ag) C*12m 0.376512 0.300892 b0.217 b0.170 0.251 0.042 0.49 0.46 0.7992
074438.61+291222.8 11.94 12.53 ag) D01 0.0885372 0.0684971 b0.0420 b0.0390 0.224 0.013 0.32 0.45 0.7737
093044.09+320916.8 15.6716.53 zg) R01 0.504562 0.375771 b0.165 b0.199 0.141 0.213 0.41 0.40 0.7447
094051.03+345205.2 14.44 15.34 zg) R01 0.4598247 0.3415975 b0.183 b0.050 0.170 0.202 0.37 0.38 0.7429
105408.01-580421.2 14.52 15.03 ag) D01 0.1932659 0.1475255 a0.0070 a0.1175 0.071 0.096 0.44 0.50 0.7633
111130.57-632636.4 12.66 13.00 ag) D12n 0.15607022 0.1247588 a0.1060 a0.0460 0.088 0.046 0.43 0.48 0.7994
143130.85+225023.4 15.48 16.15 zg) R01 0.4952015 0.3691332 b0.124 b0.033 0.067 0.217 0.48 0.39 0.7454
151609.22+320007.3 15.70 16.73 zg) R01 0.4706323 0.3499155 b0.130 b0.224 0.193 0.232 0.39 0.37 0.7435
160331.49-494754.4 13.86 14.46 ag) D012 0.2194880 0.1668487 0.1334800 b0.0400 b0.0615 b0.1111 0.068 0.161 0.013 0.45 0.54 0.50 0.7602 0.8000
171059.14-351034.8 14.09 14.40 ag) D01 0.1232822 0.09510855 a0.0095 a0.0040 0.019 0.083 0.49 0.66 0.7715
185513.28+081813.4 17.43 18.28 zr) C01 1.86705 1.34230 b0.16 b0.46 0.190 0.084 0.28 0.43 0.7189
202946.51+374539.5 14.65 15.31 zr) C01 4.2972 2.9905 b4.08 b2.07 0.179 0.070 0.35 0.45 0.6959
211839.91+504732.9 15.09 16.09 zg) C01 2.99683 2.11870 b0.35 b2.07 0.423 0.023 0.26 0.50 0.7070
Table 2. Comments for new M MRP variables
MMRP Comments MMRP Comments
001 1,2,3 026 13,15,29,42
002 1,4,5 027 4,5,43,44
003 1,2,6 028 13,16,45,46
004 5,7 029 13,47,48
005 1,5,8,9,10,11 030 12,13,15,49
006 1,2,6,12 031 13,29,35,50
007 13,14,15,16,17 032 5,13,51
008 5,7,9,12 033 13,25,52
009 7,9,16,18,19,20 034 13,14,15,23
010 9,16,21,22 035 13,53
011 4,5,20,21,23,24 036 21,34,54,55,56,57
012 13,15,25 037 10,13,14,15,29
013 1,26 038 13,15,29
014 12,27 039 13,14,15,29,31,58
015 13,16,28,29 040 1,4,5,34
016 13,30 041 14,15,16,29
017 1,2,6,16 042 4,5,31,59
018 13,15,29,31 043 7,18,60
019 13,15,25,29,32,33 044 13,15,25,61
020 13,15,29,34 045 10,13,14,15,62
021 29,35,36,37 046 5,7,63
022 13,15,17,29,38 047 7,64
023 13,17,29,39 048 7,18,65
024 13,15,29,40 049 13,14,15,16,29,66
025 12,41 050 7,18,67
Table 2a. Comments for known multi-mode variables
MMRP J
044322 054223 074438 093044 094051 105408 111130. 143130. 151609. 160331 171059. 185513. 202946 211839.
93+465703.6
13+275647.6
61+291222.8
09+320916.8
03+345205.2
01-580421.2
57-632636.4
85+225023.4
22+320007.3
49-494754.4
14-351034.8
28+081813.4
51+374539.5
91+504732.9
Comments
5,16,68,69
5,9,16,70,71
13,14,15,23,72
1,4,16,45,73,74,75
4,7,10,17,45,74,76,77
13,15,79
13,15,35,79,80
1,2,4,16,45,73,77,81,82
1,4,10,45,74,76,77,83
13.29.35.79.84 13,29,79,85 68,69
55.56.68.69.85
34.55.68.69.86
Comments.
1. Monoperiodic RRC in ZTF Catalog (Chen et al., 2020).
2. Monoperiodic RRC in Gaia DR3 Catalog (Gaia Collaboration, 2022).
3. MMRP-001. Large amplitude modulation of the second-overtone mode f2. The amplitudes in the Table are for the first interval of ZTF observations, JD 2458219-2458540; for the next observation interval, JD 2458607-2459766, the amplitudes of the oscillations are as follows: fi: A/2 is 0.109 (zr), 0.161 (zg); f2: A/2 is 0.006 (zr), 0.011 (zg).
4. Monoperiodic RRC in ASAS-SN Catalog (Jayasinghe et al., 2018, 2019a, 2019b, 2020, 2021).
5. Monoperiodic first-overtone DCEP in Gaia DR3 Catalog.
6. Monoperiodic RRC in Gaia DR2 Catalog (Gaia Collaboration, Brown, et al., 2018).
7. Monoperiodic RRAB in ZTF Catalog.
8. Monoperiodic RRc in GCVS (Samus et al., 2017).
9. Monoperiodic RRAB in ASAS-SN Catalog.
10. Variable in ATLAS catalog (Heinze et al., 2018). Class of variability "MSINE" (stars showing modulated sinusoids).
11. Monoperiodic RRC in the Czech Variable Star Catalogue (Skarka et al., 2017).
12. Variable in ATLAS catalog. Class of variability "dubious" (the star might not be a real variable).
13. Monoperiodic HADS in ASAS-SN Catalog.
14. Monoperiodic DSCT in ZTF Catalog.
15. Monoperiodic "main-sequence oscillator", or "DSCT/GDOR/SXPHE" type, in Gaia DR3 Catalog.
16. Variable in ATLAS catalog. Class of variability "MPULSE" (stars showing modulated pulsations).
17. Data from 1SWASP were used to improve the light elements.
18. Monoperiodic RRAB in Gaia DR3 Catalog.
19. MMRP-009. The light elements for the 1SWASP data: fi: HJD(max) = 2454420.373 + 0d48136 xE;
f2: HJD(max) = 2454420.240 + 0d38565 xE.
20. Blend in 1SWASP data.
21. Monoperiodic variable in ZTF suspected variables catalog (Chen et al., 2020). Type not determined.
22. MMRP-010. Equidistant quadruplet in fact: fi - f0 = 1.006209, f2 - fi = 1.006210, f3 - f2 = 1.006216.
23. Variable in ATLAS catalog. Class of variability "PULSE" (pulsating stars showing the classic sawtooth light curve, regardless of period).
24. MMRP-011. Light elements for the 1SWASP data: fi: HJD(max) = 2454100.165 + 0d37202 xE;
f2: HJD(max) = 2454100.011 + 0d29826 xE;
25. Monoperiodic DSCT in ASAS-3 Catalog of Variable Stars, Pojmanski (2002).
26. RR Lyrae star (RR) in Gaia DR3 Catalog.
27. HADS(B) star in VSX database. Period of the dominating mode is given, a second period is not given.
28. Monoperiodic EW star in ZTF Catalog.
29. Monoperiodic "short-timescale source" in Gaia DR3 Catalog.
30. MMRP-016. Amplitude modulation of the second-overtone mode, f2. The Tables give mean amplitude (for the whole observation interval). Mode-switching is not excluded, type D12^D1. In g band, three time intervals were studied:
I: JD 2458100-2458700, A = 0.036; II: JD 2458700-2459400, A = 0.014; III: JD 2459400-2459966, A > 0.007.
31. Variable in ATLAS catalog. Class of variability "CBF" (close binary, full period).
32. Monoperiodic eclipsing variable in the Catalina Surveys Southern periodic variable star catalogue (Drake et al., 2017).
33. MMRP-019. Amplitide modulation of the second-overtone mode, f2. Periods Pi and P2 possibly vary, the light elements are given separately for two time intervals, for the V band (JD 2456776-2458382) and g band (JD 2458031-2460049). Elements for V-band ASAS-SN data:
fi: HJD(max) = 2457777.1590 + 0d 1633823 xE; f2: HJD(max) = 2457777.1350 + 0d 1303228 xE.
34. Variable in ATLAS catalog. Class of variability "IRR" (irregular variable).
35. Variability was detected in the GDS catalog (Hackstein et al., 2015).
36. Monoperiodic SR variable in ASAS-SN Catalog.
37. MMRP-021. A second identification in the USN0-B1.0 catalog is possible, USNO-B1.0 0366-0148328.
38. MMRP-022. Additional non-radial pulsation with the following light elements, according to ASAS-SN data:
for V-band, JD 2457424-2458326: HJD(max) = 2457878.083 + 0d 110475 xE; for g-band, JD 2458282-2460046: HJD(max) = 2459292.100 + 0d 110468 xE;
M — m = 0.48, period ratios Pn/P1 = 0.7813, Pn/P0 = 0.5971. Semi-amplitudes An is 0.029 (aV), 0.029 (ag).
For the 1SWASP data: magnitude range 14m65-15m25; amplitudes Ao = 0.083, Ai = 0.074, An = 0.014.
39. MMRP-023. According to 1SWASP data, semi-amplitudes are A1 = 0.085 and A2 = 0.010.
40. MMRP-024. In the ASAS-SN g-band data, two possible non-radial modes with small amplitude are detected, fn and fm, periods Pn = 0d 109954 and Pm = 0d 113563. Frequency fn is also detected in 1SWASP data.
Amplitude modulation of all the radial modes. First overtone mode period varies. The light elements in the Table are for ASAS-SN g-band, JD 2458282-2460046. Elements for ASAS-SN V-band, JD 2457424-2458326:
f0: HJD(max) = 2457777.1520 + 0d 1828469 xE; f1: HJD(max) = 2457777.1053 + 0d 1401100 xE; f2 was not detected.
Elements for 1SWASP data, JD 2453860-2454239:
fo: HJD(max) = 2454141.083 + 0d 182847 xE; Ao = 0.077; f1 :HJD(max) = 2454141.031 + 0d 140108 xE; A1 = 0.094; f2: HJD(max) = 2454141.111 + 0d 112110 xE; A2 = 0.009.
Magnitude range 13m44 - 13m98 (1SWASP mag).
41. MMRP-025. Was detected as a candidate RR Lyrae star by Ivezic et al. (2000), [IGF2000] 4.
42. Monoperiodic DSCT star in the Catalina Surveys Southern periodic variable star catalogue (Drake et al., 2017).
43. Monoperiodic RRC star in ASAS-3 Catalog.
44. MMRP-027. Elements for ASAS-3 data:
f1: HJD(max) = 2453333.307 + 0d342260 xE; A1 = 0.085; f2: HJD(max) = 2453333.410 + 0d273581 xE; A2 = 0.018;
Magnitude range 11m24-11m57 (V).
45. Data from CSS and SSS were used to improve the light elements.
46. MMRP-028. According to SSS data, semi-amplitude A0 = 0.144, A1 = 0.031. Magnitude range 14m85-15m36 (CV).
47. RS Canum Venaticorum star (RS type) in Gaia DR3 Catalog.
48. MMRP-029. Periods vary. Light elements for ASAS-SN g-band are given in the Table. Elements for ASAS-SN V-band:
f0: HJD(max) = 2457777.0160 + 0d 0961740 xE ;
fi: HJD(max) = 2457777.0138 + 0d0742619 xE.
49. DSCTSXPHE star in Gaia DR2 Catalog.
50. MMRP-031. According to ASAS-SN g-band data, possible non-radial mode with Pn = 0e? 157944, or amplitude modulation (Blazhko effect) of the third-overtone mode with the period n = 42d.
51. MMRP-032. Amplitude modulation of the second-overtone mode f2, mean amplitudes (for the full time-interval) are given in the Table. Three time intervals were studied:
I: JD 2458231-2458777, A = 0.009;
II: JD 2458892-2459510, A = 0.030;
III: JD 2459610-2460050, A > 0.006.
52. MMRP-033. Periodic variable of ambiguous classification, as given in Nataf et al. (2010). In OGLE catalog, possible wrong identification with 0GLE-BLG-DSCT-06966.
Amplitude modulation of first overtone mode fi is detected in the ASAS-SN data, V and g bands. The mean amplitudes are given in the Tables (for the whole observation intervals for individual bands).
Data from ASAS-3 were used to improve the light elements. Magnitude range and amplitude according to ASAS-3 data: 11m61-12m31 (V), A0 = 0.217, A1 = 0.037.
53. MMRP-035. Data from SSS were used to improve the light elements of fundamental mode, f0. First-overtone period P1 varies. Magnitude range and amplitude according to SSS data: 14m98-15m64 (CV), A0 = 0.151; Ai = 0.073.
54. Monoperiodic rotational variable (ROT type) in ASAS-SN Catalog.
55. Monoperiodic fundamental mode 8 Cephei star (DCEP type) in Gaia DR3 Catalog.
56. MIRA_SR variable in Gaia DR2 Catalog.
57. MMRP-036. Blend in NSVS and ASAS-SN data. Large magnitude scattering in ZTF r-band data. Elements for NSVS data:
f0: HJD(max) = 2451402.91 + 5d 61 xE ; A0 = 0.068;
f1: HJD(max) = 2451401.55 + 3d 91 xE ; A1 = 0.025;
Magnitude range 12m09-12m34 (R).
58. MMRP-039. In V-band ASAS-SN data, JD 2456084-2458427 (earliest time-interval), second-overtone mode f2 is not detected, semi-amplitude A2 > 0.014. Possibly, it is due to large errors, or amplitude modulation is possible.
59. The variability was detected by Hartman et al. (2004), pulsating type.
60. MMRP-043. In the ZTF catalog, two periods were detected: for the r band, P = 0d8404704 corresponds to f0 (the most likely period), or for the g-band, P = 0d6179089 corresponds to f1 .
61. Variable in ATLAS catalog. Class of variability "SINE" (sinusoidal variables).
62. Monoperiodic DSCT star in GCVS.
63. Monoperiodic RRAB star in Gaia DR2 Catalog.
64. MMRP-047. Amplitude and magnitude range in the i band of ZTF data: A1 = 0.115, A2 = 0.026; 16m64-16m98 (i).
65. MMRP-048. Amplitude and magnitude range in the i band of ZTF data: A1 = 0.101, A2 = 0.024; 16m73-17m04 (i).
66. MMRP-049. Elements for 1SWASP data:
f0: HJD(max) = 2454345.442 + 0d 17941 xE; A0 = 0.033; f1: HJD(max) = 2454345.531 + 0d 13753 xE; A1 = 0.103.
Magnitude range 14m00-14m46 (1SWASP mag).
67. MMRP-050. Periods P1 and P2 possibly vary.
68. Monoperiodic DCEP variable in ZTF Catalog.
69. Multiperiodicity detected by Shah et al. (2022).
70. Monoperiodic RRAB star in GCVS.
71. MMRPJ054223.13+275647.6 = IY Tau. Double periodicity was detected by Khruslov (2018)11. In this study, I detected amplitude modulation of the second-overtone mode f2, according to ASAS-SN data. The Table gives semi-amplitude for the second g-band interval, JD 2459429-2460055. For the first g-band interval, JD 2458083-2459328, A1 = 0.274, A2 = 0.018. Period P1 varies. For the V-band, ASAS-SN data gives the following elements:
f1: HJD(max) = 2457777.140 + 0d376502 xE; f2: HJD(max) = 2457777.283 + 0d300891 xE;
V-band amplitudes in Tables are given according to data from the second V-band interval, JD 2457745-2458443. Amplitude for the first V-band interval, JD 24570082457720: A1 = 0.212, A2 > 0.006 f is not detected);
Elements according to 1SWASP data (for light curves see Khruslov, 2018): f1: HJD(max) = 2453777.214 + 0d3764978 xE; A1 = 0.168; f2: HJD(max) = 2453777.096 + 0d3009072 xE; A2 = 0.028.
72. MMRPJ074438.61+291222.8. Double periodicity was detected by Wils et al. (2012), classified as a HADS star of fundamental and first-overtone modes. Periods varys. Light elements in the Table are given for the time interval JD 2458033-2459830, ASAS-SN g band and ZTF g band.
For ASAS-SN V-band, JD 2456905-2458452, light elements are: f0: HJD(max) = 2457777.0787 + 0d0885367 xE; f1: HJD(max) = 2457777.0090 + 0d0684978 xE;
Elements for 1SWASP data:
f0: HJD(max) = 2454120.0653 + 0d0885370 xE; A0 = 0.188; f1: HJD(max) = 2454120.0228 + 0d0684974 xE; A1 = 0.016.
73. Double-mode RR Lyrae star (RRd type) in Gaia DR2 Catalog.
74. Double-mode RR Lyrae star (RRd type) in Gaia DR3 Catalog.
75. MMRP_J093044.09+320916.8. Magnitude range and semi-amplitude according to CSS data: 15m65-16m34 (CV); A0 = 0.112, A1 = 0.167.
76. Double-mode RR Lyrae variable (RRd type) in the Catalina Surveys periodic variable stars catalog (Drake et al., 2014).
77. Double periodicity detected by Huemmerich and Bernhard (2014) corresponds to 2012. Type RRd.
78. MMRPJ094051.03+345205.2 Magnitude range and semi-amplitude:
according to CSS data: 14m43-15m 15 (CV); A0 = 0.135, A1 = 0.152;
according to 1SWASP data: 14m6-15m6 (1SWASP mag), A0 = 0.164, A1 = 0.192.
79. The variable is in the OGLE 6 Scuti stars database12, Pietrukowicz et al. (2020).
11 http://www.inasan.ru/wp-content/uploads/2018/12/Boyarchuk.pdf#page=57
12 https://ogledb.astrouw.edu.pl/ ogle/OCVS/dsct_query.php
80. MMRP_J111130.57-632636.4. According to ASAS-SN g-band data, there is additional non-radial oscillation, Pn = 0d 12072463 ; An = 0.008.
81. Monoperiodic RRC star in the Catalina Surveys periodic variable stars catalog (Drake et al., 2014).
82. MMRP_J143130.85+225023.4. Magnitude range and semi-amplitude according to CSS data: 15m35-15m92 (CV), A0 = 0.040, Ai = 0.172.
83. MMRP_J151609.22+320007.3. Magnitude range and semi-amplitude according to CSS data: 15m76-16m51 (CV), A0 = 0.117, Ai = 0.155.
84. MMRPJ160331.49-494754.4. Second-overtone mode f2 is not detected in ASAS-SN V-band.
Possible non-radial oscillation fn detected in ASAS-SN g and V bands, Pn = 0d 1262036, An = 0.012 (ag); this frequency is possibly a one-day alias mode to third overtone mode,
fn = f3 - 1.
In ASAS-SN V-band, two other oscillation with the periods close to Pi, 0d 1345739 and 0d 1349735, are possibly detected.
85. Blend in ASAS-SN data.
86. Monoperiodic DCEP star in ASAS-SN Catalog. 5.2 Light curves
An example of light curves for one of the stars, MMRP-049, is displayed in Fig. 1. Top panels present data folded with the fundamental-mode and first-overtone periods. Bottom panels show the same curves after prewhitening the other oscillation (if fi+f0, fi-f0 and fi+2f0 interaction frequencies or non-radial frequencies were excluded, it is also noted). Along with the light curves, we present power spectra of the double-mode variables, for the raw data and after subtraction of the dominant mode (first-overtone oscillations for MMRP-049). The structure of the power spectra shows that the secondary periods are real.
The light curves from the ASAS-SN surveys are available online in the html version of this paper as a zip archive (see Section 2). The light curves are given in the format displayed in Fig. 1. A similar and more complete format is used for triple- and quadruple-mode variables.
6 Discussion
6.1 The Petersen diagram
Among the 50 stars with multi-periodicity discovered in this study, there are 15 Classical Cepheids (two stars of the C01 type, 8 stars of the C12 type, and 5 stars of the C*12 type); four RR Lyrae stars of the R01 type; 31 high-amplitude ô Scuti stars (double-mode: 9 D01 stars, 12 D12 stars, 4 D23 stars; triple-mode: 4 D012 stars and one D123 star; and one quadruple-mode star of the D0123 type).
Among the 14 known multi-periodic stars studied in this paper, there are 5 Classical Cepheids (three of C01 type, one of C12 type, and one of C*12 type); four RR Lyrae stars of R01 type; 5 high-amplitude ô Scuti stars (3 of D01 type, one of D12 type, one of D012 type).
In this paper, the distribution by variability type is not statistically significant. In fact, in the sample of multi-periodic variable stars, the largest fraction belongs to R01 stars. The number of D01 stars is slightly lower. Next in number are the first- and
Figure 1.
The light curves and power spectra of the star MMRP-049 (D01 type) from g-band ASAS-SN data.
second-overtone variables of different types (D12 and C12) and C01 Cepheids. For the present paper, I selected the rarest and most interesting objects encountered in my search for multi-periodicity.
The Petersen diagram for all MMRP variables studied in this paper is displayed in Fig. 2.
Ps/PL
0.86
0.8d 0.82 0.80 0,73 0.76 0,74 0,72 0.70 0 63 0.66
-1,5 -1.0 -0,5 0,0 0.5 1,0
log PL
Figure 2.
The Petersen diagram for the multi-periodic stars of the present study. Blue circles are double-mode variables, green triangles are triple-mode variables, and red squares are quadruple mode variables.
6.2 Asymmetry inversion for light curves of 5 Scuti stars
In the photometric data of recent surveys, we find more and more 5 Scuti stars with light-curve asymmetry opposite compared to brightness variations of typical pulsating stars. Pietrukowicz et al. (2020) show four examples of phased light curves of monoperiodic 5 Scuti variables with inversion of asymmetry (the rising part lasting longer than the fading one), and classify these stars as likely first-overtone pulsators.
In this paper, I present a confirmation of this assumption using multiperiodic stars. I detected 10 double- and multi-mode variables with one of the modes showing asymmetry inversion. Among these stars, three are of the D01 type (MMRP-22, MMRP-49, and MMRPJ171059.14-351034.8), four stars belong to the D12 type (MMRP-19, MMRP-23, MMRP-26, and MMRP-32), two stars are of the D012 type (MMRP-24 and
MMRP_J160331.49-494754.4), and one star is of the D0123 type (MMRP-10). In all these cases, the mode with asymmetry inversion is the first overtone.
An example of the light curves of one of the stars with asymmetry inversion (MMRP-49) is shown in Fig. 1.
The maximal asymmetry inversion was detected for MMRP_J171059.14-351034.8, M — m = 0? 66.
All these stars have the longest periods for 8 Scuti stars, 0d296 > P1 > 0"?095 (for four monoperiodic cases by Pietrukowicz et al., 2020, the periods are within the renge 0d 130 > Pi > 0d087).
In addition, a slight inversion of asymmetry was detected for MMRP-011, a star of the C*12 type (M — m = 0.52). MMRP-011 (P1 = 0d372, b = +0°.9) is similar to the D12 star MMRP-032 (Pi = 0.296, b = +2°.0) and to two known double-mode first- and second-overtone variables with a slight inversion of asymmetry, V798 Cyg (Pi = 0d 195, b = +4°.6) and V1719 Cyg (Pi = 0d267, b = +2°.6). Note both the morphological similarity of the light curves and the stars' similar position relative to the Galactic plane.
6.3 C*12 stars
In addition to the C12 type, I used the C*12 type that includes stars morphologically close to the C12 type (asymmetry parameter M—m = 0.50 or slightly inverted asymmetry, with a small hump at the beginning of the brightness increase), but with shorter periods (0d 45 > P1 > 0d30) characteristic of R1 stars (RRC), bordering 8 Scuti stars. All these stars are located near the Galactic plane. This classification is based on OGLE13 and Gaia DR3 catalogs (Gaia Collaboration, 2022), which classified similar stars as first- and second-overtone Cepheids. In my study, 6 stars belong to the C*12 type: MMRP005, MMRP011, MMRP027, MMRP040, MMRP042, and MMRPJ054223.13+275647.6 = IY Tau.
It should be noted that in the OGLE classification (see Soszyn'ski et al., 2020), a number of stars from the MMRP list with even shorter periods (of 8 Scuti type in my classification) are attributed to first-overtone Cepheids (MMRP002 and MMRP032). Some other variables may also be related to this type of stars (MMRP001 and MMRP010).
6.4 Amplitude modulation
For 7 variables, slow amplitude modulation (variations from one season to another) was detected. For these stars, the tabulated variability type included the letter "m" (for example, C12m, D12m, D01m). These are mainly cases of amplitude modulation of the second-overtone mode for the first- and second-overtone double-mode 8 Scuti variables (four D12m type stars: MMRP-001, MMRP-16, MMRP-19, and MMRP-32). One D01m star (MMRP-33) showed amplitude modulation of the first-overtone mode. One triple-mode 8 Scuti star of type D012m (MMRP-24) showed possible amplitude modulation of all its radial pulsation modes. Also, one C*12m Cepheid star, MMRPJ054223.13+275647.6 = IY Tau, showed amplitude modulation of the second-overtone mode.
In some cases, a periodic amplitude variation is possible, but, in a number of cases, it also can be mode switching.
Two examples of amplitude modulation are shown in Figs. 3 and 4. MMRP-033 it a possible mode-switching case. MMRP-032 is possibly a case of periodic amplitude variations (during short time intervals of observations, the star shows the "episodic" multiperiodicity; for intervals and variability amplitudes, see Comments to Table 1).
13 https://ogledb.astrouw.edu.pl/ ogle/OCVS/ceph_query.php
Figure 3.
The amplitude modulation of MMRP-033. Top panels: g-band ASAS-SN data folded with the fundamental-mode period P0 in the two time-intervals; Bottom panel: amplitude variations of the firstovertone mode in the g and V bands of ASAS-SN data.
Figure 4.
The amplitude modulation of MMRP-032 in three time intervals (see Comments). Left panels: g-band ASAS-SN data folded with the first-overtone mode period Pi; right panels: g-band ASAS-SN data folded with the second-overtone mode period P2; bottom panel: the power spectra of the second-overtone mode.
6.5 Triple- and quadruple-mode 5 Scuti stars
In my study, 6 triple-mode variables were detected. Five of these stars belong to the D012 type: MMRP-012, MMRP-014, MMRP-024, MMRP-039, MMRPJ160331.49-494754.4. In the case MMRP_J160331.49-494754.4, the second-overtone mode was not earlier known (in the OGLE database, the star was classified as a variable with two periods, those of the fundamental and first-overtone modes). The sixth star, MMRP-002, belongs to the D123 type.
In all cases of the five D012 stars, with a single exception of MMRP-014, the firstovertone mode dominates. The first-overtone mode also dominates for the D123 star MMRP-002. In two cases, the light curve of the first-overtone oscillation showed asymmetry inversion.
One case, MMRP-010, is a quadruple-mode 5 Scuti star of the D0123 type. Additionally, it is an equidistant quadruplet with the frequency differences fi - f0 = f2 - fi = f3 — f2 = 1.0062. The light curve of the first-overtone oscillation of this star also shows inverted asymmetry.
Netzel et al. (2022) presents 14 quadruple-mode 5 Scuti stars of the D0123 type from the OGLE database (Galactic bulge). Among them, no one is an equidistant quadruplet. These authors also presented the discovery of numerous triple-mode 5 Scuti star of the D013 type (221 variables), their number considerably exceeding that of the D012 stars (145 variables). In my study, no D013 stars were detected.
6.6 D23 variables
In this paper, I present my detection of four double-mode 5 Scuti stars pulsating in the second- and third-overtone modes, type D23 (MMRP-020, MMRP-031, MMRP-041, and MMRP-045 = V2702 Cyg). Earlier, I found two stars of this type. The first of them is FH Cir (Khruslov, 2010, first classification as a 5 Scuti star with nonradial pulsations; P2 = 0d 1522950, P3/P2 = 0.8279; the star was reclassified as a D23 variable by Khruslov, 2016, PhD dissertationi4). The second of them is V3124 Cyg (Khruslov, 2014, P2 = 0d 1053020, P3/P2 = 0.8342).
According to my study, the second-overtone periods of D23 stars range from 0d. 099 to 0d 190. The period ratio P3/P2 is from 0.8253 to 0.8342.
For one of the stars, MMRP-031, I detected an amplitude modulation of the third-overtone mode that can be interpreted as Blazhko effect with the period n = 42d or as a non-radial mode with a frequency close to that of the third-overtone mode, Pn = 0d. 157944. This case can be possibly classified as a D23n star, where the letter "m" in the MMRP catalog designates long-term variations and is not used for stars with Blazhko effect.
It is particularly interesting that Netzel et al. (2022) did not detect any stars of the D23 type.
Acknowledgments: The author wishes to thank Dr. V.P. Goranskij for providing his software.
14 https://www.sai.msu.ru/dissovet/Khruslov_PhD.pdf
Figure 5.
The light curves and power spectra of the star MMRP-041 (D23 type) from g-band ZTF data.
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7 Supplement Tables
Table 3. Semi-amplitudes and magnitude ranges. New MMRP stars
MMRP aV Semi-ag ampl. zr zg aV Mag. ag range zr zg
001 - - 0.102 0.159 - - 16.27- 17.12-
- - 0.046 0.060 16.66 17.63
002 0.125 0.147 0.100 0.149 14.87- 15.34- 14.55- 15.40-
0.025 0.037 0.022 0.034 15.42 16.02 14.91 15.94
0.032 0.042 0.029 0.039
003 — - 0.058 0.086 - - 17.64- 17.73-
- - 0.150 0.224 18.20 18.47
004 0.139 0.155 0.150 0.230 15.15- 15.77- 14.74- 16.12-
- 0.025 0.011 0.018 15.75 16.45 15.14 16.70
005 0.117 0.140 - 0.133 11.87- 12.26- - 12.27-
0.027 0.035 - 0.038 12.31 12.68 12.71
006 - - 0.042 0.059 - - 17.51- 17.66-
- - 0.162 0.238 18.00 18.41
007 0.107 0.109 0.076 0.118 13.86- 13.96- 13.86- 13.94-
0.034 0.038 0.025 0.036 14.27 14.37 14.11 14.32
008 0.131 0.161 0.133 0.187 15.61- 16.20- 15.16- 16.47-
0.051 0.061 0.045 0.066 16.38 17.08 15.58 17.09
009 0.206 0.254 0.165 0.257 13.98- 14.48- 13.54- 14.44-
0.027 0.040 0.029 0.043 14.63 15.25 14.00 15.11
010 0.143 0.164 0.112 0.162 14.00- 14.37- 13.68- 14.32-
0.120 0.136 0.102 0.130 14.74 15.21 14.26 15.17
0.025 0.025 0.016 0.024
0.020 0.023 0.016 0.023
011 0.132 0.163 0.128 0.193 13.44- 13.77- 13.34- 13.99-
0.014 0.022 0.015 0.022 13.83 14.30 13.68 14.48
012 0.005 0.004 - - 12.56- 12.66- - -
0.187 0.228 - - 13.04 13.24
0.013 0.018 - -
013 - - 0.127 0.155 - - 18.12- 18.92-
- - 0.155 0.199 18.81 19.88
014 - - 0.133 0.208 - - 16.65- 16.53-
- - 0.089 0.111 17.37 17.61
- - 0.023 0.036
MR
015
016
017
018
019
020
021
022
023
024
025
026
027
028
Table 3 (continued)
Semi- ampl.
aV ag zr
zg
aV
Mag.
ag
range zr
zg
0.097 0.112 0.072 0.128 0.029 0.033 0.020 0.032
0.164 0.032
0.095 0.013
0.078 0.019
0.165 0.036
0.200 0.015
0.047 0.162
0.080 0.007
0.102 0.016
0.131 0.174 0.024 0.034
0.074 0.019
0.092 0.089
0.086 0.011
0.081 0.121
0.100 0.026
0.113 0.108
0.106 0.013
0.103 0.105 0.011
0.103 0.041
0.132 0.012
0.086 0.021
0.184 0.044
0.069 0.231
0.124 0.141 0.071 0.144 0.015 0.027 0.013 0.023
0.093 0.180 0.020 0.038
0.134 0.057
13.93- 14.1214.24 14.48
14.01- 14.1414.50 14.70
13.5013.86
12.6612.90
14.6015.15
12.7813.04
13.2513.79
11.2211.48
15.2015.95
13.6814.10
12.9113.22
14.7415.38
12.9913.30
13.5014.03
11.4611.75
15.5216.25
14.0014.24
16.1716.69
13.5013.74
12.46- 12.66- 12.6512.92 13.16 12.99
12.76- 13.24- -
13.03 13.57
13.58- 13.7313.87 14.11
14.1114.50
16.3617.09
13.6814.05
12.7813.32
17.91- 17.9518.39 18.50
Table 3 (continued)
MMRP aV Semi-ag ampl. zr zg aV Mag. ag range zr zg
029 0.053 0.042 0.068 0.044 - - 13.7614.08 14.1214.50 - -
030 0.116 0.058 0.132 0.069 0.090 0.052 0.141 0.078 14.6615.18 14.7615.34 14.8415.23 14.8315.32
031 0.126 0.030 0.143 0.032 - - 13.8614.29 14.2914.78 - -
032 0.103 0.022 0.128 0.015 - - 13.1513.48 13.6013.97 - -
033 0.199 0.056 0.240 0.036 - - 11.4912.12 11.6912.35 - -
034 0.098 0.033 0.120 0.045 0.084 0.029 0.119 0.040 13.6314.03 13.7814.25 13.7313.99 13.8514.25
035 0.162 0.067 0.203 0.076 - - 14.8915.77 14.9915.86 - -
036 0.129 0.067 0.131 0.064 0.120 0.061 0.195 0.104 13.6914.15 14.6015.21 12.7013.26 14.9715.66
037 0.073 0.049 0.081 0.056 0.059 0.041 0.086 0.060 14.4514.80 14.9015.35 14.0314.26 14.9315.28
038 0.057 0.025 0.071 0.032 - - 14.2014.50 14.4014.72 - -
039 0.058 0.106 >0.014 0.071 0.130 0.018 0.042 0.076 0.011 0.070 0.129 0.015 14.4615.00 14.7015.38 14.2114.57 14.7215.24
040 0.130 0.020 0.161 0.025 0.117 0.016 0.178 0.024 14.0814.54 14.6715.25 13.5913.96 14.8715.37
041 0.094 0.030 0.121 0.039 0.091 0.027 0.153 0.045 14.8515.40 15.3516.00 14.7115.12 15.5016.01
042 0.136 0.020 0.161 0.026 - - 11.6312.04 11.8912.34 - -
Table 3 (continued)
MMRP aV Semi-ag ampl. zr zg aV Mag. ag range zr zg
043 0.127 0.189 17.26- 19.7-
- - 0.117 0.185 18.06 21.0
044 0.080 0.104 - - 11.49- 11.73- - -
0.018 0.021 - - 11.73 12.05
045 0.075 0.088 0.052 0.089 12.47- 12.72- 12.40- 12.73-
0.022 0.027 0.016 0.029 12.72 13.01 12.59 13.02
046 — - 0.147 - - - 18.16- 20.9-
- - 0.022 - 18.64 21.7
047 — - 0.151 0.233 - - 17.60- 19.5-
- - 0.033 0.058 18.09 20.2
048 — - 0.135 0.201 - - 17.80- 19.7-
- - 0.031 0.045 18.20 20.4
049 0.042 0.045 0.029 0.047 13.77- 13.90- 13.84- 13.96-
0.143 0.150 0.109 0.156 14.25 14.41 14.16 14.43
050 - - 0.162 0.227 15.30- 15.92- 15.35- 16.55-
— - 0.040 0.058 15.75 16.45 15.90 17.34
Table 3a. Semi-amplitudes and magnitude ranges. Known multi-mode _variables_
MMRP_J aV Semi-ag ampl zr zg aV Mag. ag range zr zg
044322.93+465703.6 0.245 0.047 0.270 0.063 0.185 0.043 0.261 0.062 14.1514.89 14.7915.72 13.5514.08 14.7515.58
054223.13+275647.6 0.206 0.024 0.251 0.042 - 0.240 12.4813.08 12.8913.61 - 12.9913.53
074438.61+291222.8 0.201 0.012 0.224 0.013 - 0.233 0.013 11.9212.42 11.9412.53 - 11.9412.50
093044.09+320916.8 0.115 0.186 0.135 0.206 0.112 0.157 0.141 0.213 15.6516.70 15.6616.75 15.6616.30 15.6716.53
094051.03+345205.2 0.147 0.178 0.188 0.205 0.125 0.148 0.170 0.202 14.3715.32 14.4015.42 14.5015.15 14.4415.34
105408.01-580421.2 0.059 0.074 0.071 0.096 - - 14.2414.66 14.5215.03 - -
111130.57-632636.4 0.068 0.036 0.088 0.046 - - 12.4012.71 12.6613.00 - -
143130.85+225023.4 0.063 0.204 0.079 0.239 0.045 0.157 0.067 0.217 15.416.1 15.516.4 15.4515.93 15.4816.15
151609.22+320007.3 0.152 0.150 0.191 0.216 0.132 0.151 0.193 0.232 15.616.5 15.616.8 15.7816.47 15.7016.73
160331.49-494754.4 0.058 0.133 0.068 0.161 0.013 - - 13.4313.94 13.8614.46 - -
171059.14-351034.8 0.018 0.069 0.019 0.083 - - 13.5413.82 14.0914.40 - -
185513.28+081813.4 - - 0.190 0.084 0.316 0.144 - - 17.4318.28 19.621.1
202946.51+374539.5 0.021 0.011 - 0.179 0.070 0.291 0.107 13.8814.05 - 14.6515.31 17.4018.42
211839.91+504732.9 0.364 0.022 0.424 0.030 0.276 0.014 0.423 0.023 14.2315.25 15.1016.29 13.5114.19 15.0916.09
le 4
MM
001
002
003
004
005
006
007
008
009
010
011
012
013
014
015
016
017
018
019
020
021
022
023
024
025
026
027
028
029
030
031
032
033
034
035
036
037
038
039
040
041
042
043
044
indices and Galactic latitudes. New MMRP-stars
- K, B - V, g' - r', g - V, g - r b, deg
MASS APASS APASS ASAS-SN ZTF
0.59 1.22 0.93 0.92 +0.5
0.59 0.86 0.62 0.53 0.97 -0.7
- - - - 0.21 -46.4
0.82 1.50 1.30 0.67 1.43 +0.4
0.47 0.89 0.71 0.38 - -3.4
0.25 - - - 0.33 -12.9
0.17 0.33 0.18 0.12 0.17 -13.6
0.81 1.47 1.29 0.69 1.42 +3.8
0.55 1.14 1.02 0.58 1.01 +0.3
0.47 0.91 0.72 0.45 0.82 -2.9
0.49 0.83 0.70 0.40 0.74 +0.9
0.18 0.34 0.17 0.18 - -25.1
- - - - 0.87 -4.7
- 0.41 0.11 - 0.16 +26.8
0.23 0.46 0.25 0.19 0.22 +6.7
0.25 0.42 0.27 0.17 - -19.0
0.58 0.46 0.20 - 0.37 +5.1
0.21 0.50 0.31 0.22 0.28 +8.6
0.30 0.67 0.44 0.28 - -12.2
0.26 0.44 0.28 0.22 0.32 +5.0
0.92 1.14 1.06 0.51 - -2.6
0.24 0.50 0.32 0.23 - +9.4
0.23 0.52 0.32 0.24 - + 11.0
0.28 0.55 0.41 0.24 - +9.7
- - - - 0.08 +51.6
0.19 0.45 0.26 0.21 - +21.8
0.29 -0.14 ? 0.47 0.25 - +3.7
0.31 0.67 0.52 0.28 - +22.8
0.58 0.71 0.57 0.38 - +11.7
0.22 0.22 -0.02 0.14 0.05 +30.0
0.49 0.91 0.70 0.42 - -0.5
0.59 1.00 0.87 0.47 - +2.0
0.32 0.60 0.54 0.24 - -3.6
0.13 0.39 0.18 0.17 0.22 +9.9
- 0.34 -0.01 0.13 - -19.8
1.04 2.39 2.18 1.01 2.36 + 1.0
0.51 1.07 0.93 0.53 0.99 -1.1
0.25 0.49 0.29 0.22 - -27.0
0.41 0.62 0.47 0.30 0.61 +5.3
0.57 1.42 1.23 0.67 1.38 +2.9
0.43 1.03 0.90 0.62 0.85 +2.4
0.28 0.51 0.36 0.32 - +7.1
1.26 - - - 2.63 -0.0
0.35 0.67 0.42 0.29 - -4.0
Table 4 (continued)
MMRP J - K, B - V, g - V, g - r b, deg
2MASS APASS APASS ASAS-SN ZTF
045 0.25 0.75 0.54 0.28 0.38 -0.5
046 1.35 - - - 2.85 -1.0
047 1.05 - - - 1.95 +4.3
048 1.07 - - - 2.04 +2.5
049 0.23 0.45 0.20 0.15 0.22 -12.7
050 0.73 - 1.52 0.67 1.36 +2.3
Table 4a. Color indices, and Galactic latitude. Known multi-mode variables
MMRP J - K, B - V, g'- r', g - V, g - r, b, deg
2MASS APASS APASS ASAS-SN ZTF
044322.93+465703.6 0.81 1.58 1.42 0.70 1.37 +0.6
054223.13+275647.6 0.58 1.06 0.89 0.48 - -1.1
074438.61+291222.8 0.20 0.27 0.06 0.09 - +23.7
093044.09+320916.8 0.12 0.18 0.00 0.17 0.16 +46.5
094051.03+345205.2 0.26 0.20 0.19 0.11 0.11 +48.8
105408.01-580421.2 0.37 0.72 0.57 0.32 - + 1.3
111130.57-632636.4 0.44 0.69 0.55 0.31 - -2.7
143130.85+225023.4 0.23 0.46 0.15 0.20 0.14 +67.0
151609.22+320007.3 0.19 0.17 0.03 0.15 0.13 +58.3
160331.49-494754.4 0.59 0.84 0.72 0.48 - +2.1
171059.14-351034.8 0.53 1.13 1.06 0.57 - +2.6
185513.28+081813.4 1.19 - - - 2.48 +2.9
202946.51+374539.5 1.41 - - - 2.99 -0.8
211839.91+504732.9 1.07 1.90 1.73 0.92 1.86 +0.9
