1 INTRODUCTION
Pre-main sequence (PMS) stars are newly formed objects located above the main sequence on the Hertzsprung–Russell diagram. Depending on their initial mass, these stars reach the main sequence for different time scales. One of the most important features of the PMS stars is their photometric variability. PMS stars are important objects for study of the early stages of the stellar evolution and for testing the stellar evolution scenarios.
PMS stars with low masses (M ⩽ 2 M⊙) are named T Tauri stars (TTS). The first systematic study of such young stellar objects (YSOs), as a separate class with prototype the star T Tauri, was made by Joy (Reference Joy1942; Reference Joy1945). TTS are associated with obscured regions, molecular clouds and dark nebulae and are grouped in T associations. These objects show strong irregular photometric variability and emission line spectra. TTS are separated into two subclasses − Classical T Tauri stars (CTTS), which are surrounded by massive accreting circumstellar disks, and weak-line T Tauri stars (WTTS) without evidence for disk accretion (Bertout Reference Bertout1989; Ménard & Bertout Reference Ménard, Bertout, Lada and Kylafis1999).
The more massive (2 M⊙ ⩽ M ⩽ 8 M⊙) PMS stars are known as Herbig Ae/Be stars (HAEBES). The two types PMS stars − TTS and HAEBES are still contracting towards the main sequence and their main characteristic is the photometric and spectroscopic variability, discovered at the beginning of their study.
TTS show various types of stellar activity. According to Herbst et al. (Reference Herbst, Eisloffel, Mundt, Scholz, Reipurth, Jewitt and Keil2007), the variability of WTTS is due to cool spots or groups of spots on the stellar surface. The photometric amplitudes of this variability are about 0.03–0.3 mag, but in extreme cases reach 0.8 mag in the V-band. The variability of WTTS can also be due to flare-like variations in B- and U-band. Flares are random with different sized amplitudes, as there is no periodicity. Usually, the rise of brightness is quick and occurs over short time scales. CTTS often shows irregular variations with larger photometric amplitudes up to 2–3 mag, associated with high variable accretion from the circumstellar disk onto the stellar surface. The variability of CTTS also can be due to rotating hot spots on the stellar surface.
The large amplitude drops in the brightness of the PMS stars are commonly observed in the early types of TTS and HAEBES. These objects show non-periodic deep Algol-type minima and amplitudes up to 2.8 mag in V-band. The observed drops in the brightness last from days to some weeks and are caused by circumstellar dust or clouds obscuration (Voshchinnikov Reference Voshchinnikov1989; Grinin et al. Reference Grinin, Kiselev, Minikulov, Chernova and Voshchinnikov1991; Herbst et al. Reference Herbst, Eisloffel, Mundt, Scholz, Reipurth, Jewitt and Keil2007). This group of PMS objects with intermediate mass is known as UXors and their prototype is the star UX Orionis. In very deep minima, the colour indixes of UXors often becomes bluer (so called ‘blueing effect’ or ‘colour reverse’) (see Bibo & Thé (Reference Bibo and Thé1990)). It is generally accepted that the origin of observed drops in the brightness and the bluing effect are due to variations of the column density of dust in the line of sight to the star (Dullemond et al. Reference Dullemond, van den Ancker, Acke and van Boekel2003).
The outbursts of the PMS stars with large amplitude are grouped into two types − FUors, with prototype the star FU Orionis, and EXors, with prototype the star EX Lupi (Herbig Reference Herbig1989). During the quiescence state, the FUors and EXors are normally accreting CTTS. The outbursts of both types of eruptive PMS stars are generally attributed to a sizable increase in accretion rate from the circumstellar disk onto the stellar surface.
The PMS stars included in the present study are located in the dense molecular cloud L935, known as ‘Gulf of Mexico’, between North America (NGC 7000) and Pelican Nebula (IC 5070), in the vicinity of the new FUor star V2493 Cygni (HBC 722) erupted in 2010 (Semkov et al. Reference Semkov, Peneva, Munari, Milani and Valisa2010, Reference Semkov2012, Reference Semkov, Peneva, Ibryamov and Dimitrov2014; Miller et al. Reference Miller2011). NGC 7000 and IC 5070 are thought to be parts of a single large HII region W80. The distance to this region, determined by Laugalys & Straižys (Reference Laugalys and Straižys2002) is 600 pc. ‘Gulf of Mexico’ is a region with active star formation and contains many YSO (Armond et al. Reference Armond, Reipurth, Bally and Aspin2011; Findeisen et al. Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013; Bally et al. Reference Bally, Ginsburg, Probst, Reipurth, Shirley and Stringfellow2014). The stars FHO 26, FHO 27, FHO 28, and FHO 29 are revealed as large amplitude variables in the study of Findeisen et al. (Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013). V1929 Cyg is reported as flare star from UV Ceti type by Rosino, Tsvetkov, & Tsvetkova (Reference Rosino, Tsvetkov and Tsvetkova1987).
The present paper is a part of our long-term photometric study of the PMS stars in the region of ‘Gulf of Mexico’. The results from our previous studies of PMS stars in this field have been published in Semkov et al. (Reference Semkov, Peneva, Munari, Milani and Valisa2010, Reference Semkov2012, Reference Semkov, Peneva, Ibryamov and Dimitrov2014), Poljančić Beljan et al. (Reference Poljančić Beljan, Jurdana–Šepić, Semkov, Ibryamov, Peneva and Tsvetkov2014), and Ibryamov, Semkov, & Peneva (Reference Ibryamov, Semkov and Peneva2015).
2 OBSERVATIONS AND DATA REDUCTION
The presented data from photometric observations were performed during the period from 1997 June to 2014 December, in two astronomical observatories, with four telescopes. These are the 2-m Ritchey-Chrétien-Coudé (RCC), the 50/70-cm Schmidt and the 60-cm Cassegrain telescopes of the Rozhen National Astronomical Observatory of the Bulgarian Academy of Sciences and the 1.3-m Ritchey-Chrétien (RC) telescope of the Skinakas ObservatoryFootnote 1 of the University of Crete (Greece).
The observations were performed with eight different types of CCD cameras Photometrics AT200 and VersArray 1300B at the 2-m RCC telescope; Photometrics CH360 and ANDOR DZ436-BV at the 1.3-m RC telescope; SBIG ST-8, SBIG STL-11000M, and FLI PL16803 at the 50/70-cm Schmidt telescope; FLI PL09000 at the 60-cm Cassegrain telescope. The technical parameters and specifications of the used CCD are summarized in Table 1.
Table 1. CCD cameras used and their technical parameters and specifications.
awith focal reducer.
The photometric limit of our data obtained with the 2-m RCC and the 1.3-m RC telescopes in B- and V-band is about 20.5 mag and for the data collected with the 50/70-cm Schmidt and the 60-cm Cassegrain telescopes is about 19.5 mag.
All frames were taken through a standard Johnson–Cousins set of filters. The total number of the nights used for observations is 292. All frames obtained with the VersArray 1300B, Photometrics CH360, and ANDOR DZ436-BV cameras are bias frame subtracted and flat field corrected. The frames obtained with the SBIG ST-8, SBIG STL-11000M, FLI PL16803, and FLI PL9000 cameras are dark frame subtracted and flat field corrected.
The photometric data were reduced by idl package (standard subroutine daophot). As a reference, the BVRI comparison sequence reported in Semkov et al. (Reference Semkov, Peneva, Munari, Milani and Valisa2010) was used. All data were analysed using the same aperture, which was chosen to have a 4-arcsec radius, while the background annulus was taken from 9 to 14 arcsec.
The average value of the errors in the reported magnitudes are 0.01–0.05 mag for I- and R-band data, 0.02–0.08 mag for V-band data and 0.03–0.11 mag for B-band data.
3 RESULTS AND DISCUSSION
The results from long-time BVRI photometric observations of the PMS stars FHO 26, FHO 27, FHO 28, FHO 29, and V1929 Cyg are presented in the paper. Figure 1 shows a three-colour image of the field of ‘Gulf of Mexico’, with marked positions of the stars from our study and the recently erupting FUor star V2493 Cyg. The image was obtained on 2014 August 19 with the 50/70-cm Schmidt telescope of Rozhen NAO.
Figure 1. A three-colour image of the field of ‘Gulf of Mexico’, obtained with the Schmidt telescope of Rozhen NAO on 2014 August 19. The program stars and the recently erupting FUor star V2493 Cyg are marked.
The stars from our study shows bursts and/or fades events in their light curves. These events are defined as follows. In the case that the star most of the time spends at high light during our study, the declines in the brightness are interpreted as fades. Respectively, if the star most of the time spends at a low light, the observed increases in the brightness are interpreted as bursts.
3.1. FHO 26
The star FHO 26 (2MASS J20565934+4347530) is included in the list of YSO candidates published in Guieu et al. (Reference Guieu, Rebull, Stauffer, Hillenbrand and Carpenter2009). The authors measured B = 20.195, V = 18.747 and I = 15.963 mag of the star. According to Findeisen et al. (Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013), FHO 26 shows bursts events, which are repeated every few weeks.
Findeisen et al. (Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013) presented the light curve in R-band of FHO 26 for the period 2009–2012 and described ~ 0.7 mag burst events in 2010 and 2011, lasting 4–5 d each and separated by 10–30 d. During 2012, the star has shown only two short bursts. The spectrum of FHO 26 taken in 2012 July by Findeisen et al. (Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013) shows a M4.5 photosphere with Hα in emission.
The VRI light curves of FHO 26 from our CCD observations are shown in Figure 2. On the figure, triangles denote CCD photometric data obtained with the 50/70-cm Schmidt telescope and squares—the photometric data collected with the 60-cm Cassegrain telescope. The results of our long-term multicolour CCD observations of the star are summarised in Table A1. The columns contains date (DD/MM/YYYY format) and Julian data (J.D.) of the observations, IRV magnitudes of the star, telescope and CCD camera used.
Figure 2. CCD IRV light curves of FHO 26 for the period 2000 October–2014 December.
It can be seen from Figure 2 that during our study the brightness of FHO 26 vary around some intermediate level. The star shows both increases in the brightness with different amplitudes and short drops in the brightness. The brightness of the star during the period 2000–2014 vary in the range 15.81–16.18 mag for I-band, 17.43–18.54 mag for R-band, and 18.47–19.50 mag for V-band. In a very low light, the brightness of FHO 26 in V-band is under the photometric limit of the 50/70-cm Schmidt and the 60-cm Cassegrain telescopes. The observed amplitudes are ΔI ~ 0.40 mag, ΔR ~ 1.10 mag, and ΔV > 1.0 mag.
The star shows a large amplitude photometric variability during certain periods. The observed increases of the star’s brightness in the period 2010 August– 2011 January are with amplitudes up to 0.40 mag for R-band and up to 0.65 mag for V-band; in the period 2011 June–September with amplitudes up to 0.50 for R-band and up to 0.80 mag for V-band; in the period 2012 July–2013 January with amplitudes up to 0.40 mag for R-band and up to 0.50 mag for V-band and in the period 2014 June–August are with amplitudes up to 0.35 for R-band and up to 0.40 mag for V-band. Usually, variability with such amplitudes is an indication for the presence of hot spots on the stellar surface. The variability is produced by variable accretion from the circumstellar disk and it is typical of CTTS.
In 2002 October, 2006 July, 2009 August, 2013 April, and 2013 August, small amplitude drops in the brightness of FHO 26 are observed. The amplitudes are small (ΔR ~ 0.40 mag) and the drops are caused probably by the existence of cool spots on the stellar surface or by small irregular obscuration of the star by circumstellar material. It can be seen from Figure 2 that during the whole period of observations the total star’s brightness gradually increases (well seen in R- and V-bands). The rates of increase are ~ 0.69 × 10−2 mag yr−1 for I-band, ~ 1.79 × 10−2 mag yr−1 for R-band, and ~ 3.04 × 10−2 mag yr−1 for V-band
The measured colour indices V − I and V − R versus stellar V magnitude for the period of our observations are plotted on Figure 3. From the figure, it is seen that the star becomes redder as it fades and colour reverse was not observed. Such colour variations are typical for both WTTS and CTTS, stars with cool spots, whose variability is produced by rotation of the spotted surface. In case that the decreases in the brightness are caused by obscuration from circumstellar material, the observed amplitudes are too small to show indication for colour reverse.
Figure 3. Relationship between V magnitude and V − I and V − R colour indices of FHO 26 in the period 2000 October–2014 December.
Therefore, the long-term light curves of FHO 26 gives grounds to predict different reasons for observed variability of the star. The light curves of FHO 26 shows photometric characteristics of both WTTS and CTTS with a presence of hot and cool spots on the stellar surface. Evidences of periodicity in the brightness variability are not detected. The spectrum with Hα emission of FHO 26 (Findeisen et al. Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013) can be classified as a TTS spectrum.
3.2. FHO 27
The star FHO 27 (2MASS J20580138+4345201) is included in the list of YSO candidates by Guieu et al. (Reference Guieu, Rebull, Stauffer, Hillenbrand and Carpenter2009). The authors measured B = 20.001, V = 18.319, and I = 15.759 mag of the star. Rebull et al. (Reference Rebull2011) classify FHO 27 as a flat spectrum source.
Findeisen et al. (Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013) presented the light curve in R-band of the star for the period 2009–2012. According to the authors, FHO 27 exhibits a non-periodic multiple fading events, lasting 15–40 d and separated by 30–60 d, as fading events get shallower over the course of the decline. The authors pay attention that FHO 27 was not detected in roughly half the epochs in 2012.
The spectrum of FHO 27 taken in 2012 July by Findeisen et al. (Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013) during the stars long-term low state is typical of K7 photosphere with strong Hα, Paschen series, and CaII emission and weaker HeI, [OI], and OI lines.
The BVRI light curves of FHO 27 from our CCD observations are shown in Figure 4. In the figure, diamond denote CCD photometric data obtained with the 1.3-m RC telescope, the symbols used for the 50/70-cm Schmidt and the 60-cm Cassegrain telescopes, are as in Figure 2. The results of our long-term multicolour CCD observations of FHO 27 are summarised in Table A2. The columns contains date (DD/MM/YYYY format) and Julian data (J.D.) of the observations, IRVB magnitudes of the star, telescope and CCD camera used.
Figure 4. CCD IRVB light curves of FHO 27 for the period 2000 October–2014 December.
The brightness of FHO 27 during the period of our observations 2000–2014 vary in the range 14.36–16.31 mag for I-band, 15.58–17.93 mag for R-band, 16.68–19.26 mag for V-band, and 17.84–19.62 mag in B-band. Because of the limit of our photometric data, the deeper fading events of FHO 27 in V- and B-bands are not registered. The observed amplitudes are ΔI ~ 1.95 mag, ΔR ~ 2.35 mag, ΔV > 2.6 mag, and ΔB > 1.8 mag.
It can be seen from Figure 4 that the star usually spends most of the time at high light. During our photometric monitoring, several deep declines in the brightness of FHO 27 are registered. The drops in the brightness are non-periodic and have different duration and amplitudes. It is possible to suggest the existence of a frequent deep fading events during periods with insufficient data. Now we can identify four deep fading events, at the end of 2009–beginning 2010, at the end of 2011, in the period 2012–2013, and in the period 2013–2014.
In the early 2012, the deepest and prolonged drop in the brightness in all bands of FHO 27 begins and reaches the biggest depth in 2012 November with amplitudes 1.82 mag in I-band, 2.20 mag in R-band, and 2.38 mag for V-band. Since 2012 November the star’s brightness began to rise, continuing to late 2014, but from 2014 November new drop in the brightness started. During the prolonged fading event, some low amplitude sudden declines are also observed. Evidences of periodicity in the brightness variability of FHO 27 are not detected.
The large amplitudes of observed declines in the brightness of FHO 27 are indication of UXor-type variability and the deep fading events presumably are result of circumstellar dust or clouds obscuration. On Figure 5, the colour indices V − I, V − R, and B − V versus stellar V magnitude during the period of our observations are plotted. The figure shows evidences for colour reversal, especially for B − V index. The different shape of the observed declines gives grounds to predict a variety of obscuration reasons, clouds of proto stellar material, massive dust clumps orbiting the star or planetesimals at different stages of formation.
Figure 5. Relationship between V magnitude and the V − I, V − R, and B − V colour indices of FHO 27 in the period 2000 October–2014 December.
The light curves of FHO 27 are very similar to light curves of V521 Cyg (HBC 299), which was classified as UXor by Grankin et al. (Reference Grankin, Melnikov, Bouvier, Herbst and Shevchenko2007) and Ibryamov et al. (Reference Ibryamov, Semkov and Peneva2015). V521 Cyg is located at about 9 arcmin from FHO 27.
3.3. FHO 28
The star FHO 28 (2MASS J20582555+4353287) is included in the list of YSO candidates published in Guieu et al. (Reference Guieu, Rebull, Stauffer, Hillenbrand and Carpenter2009). The authors measured B = 21.012, V = 19.153, and I = 15.932 mag of the star. Armond et al. (Reference Armond, Reipurth, Bally and Aspin2011) includes FHO 28 in the list of Hα emission-line stars and measured V = 19.58, R = 18.11, and I = 16.81 mag of the object.
Findeisen et al. (Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013) presented the light curve in R-band of FHO 28 for the period 2009–2012 and described fades events of the star. The spectrum of FHO 28 taken in 2012 by Findeisen et al. (Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013) during the star’s strongly varying phase shows a M3 photosphere with Hα in emission and weak emission of CaII, [NII], HeI.
The BVRI light curves of FHO 28 from our CCD observations in the period 1997–2014 are shown in Figure 6. In the figure, circles denote CCD photometric data taken with the 2-m RCC telescope, the other symbols used for the 1.3-m RC, the 50/70-cm Schmidt, and the 60-cm Cassegrain telescopes are as in Figure 4. The results of our long-term multicolour CCD observations of the star are summarised in Table A3. The columns have the same contents as in Table A2.
Figure 6. CCD IRVB light curves of FHO 28 for the period 1997 June–2014 December.
It can be seen from the Figure 6 that FHO 28 spends most of the time at high light. The star exhibit strong irregular multiple fading in all bands with different amplitudes. The periods of decline in the brightness are relatively short, sometimes we have only one photometric point in the deep minimum. The brightness of FHO 28 during the period of our observations 2000–2014 vary in the range 15.42–17.07 mag for I-band and 16.89–19.38 mag for R-band. The observed amplitudes are 1.65 mag for I- and 2.49 mag for R-bands, respectively. Because of the limit of our photometric data, the deeper drops in the brightness of FHO 28 in V- and especially in B-bands are not registered. We have only some photometric points of the star in B-band collected with the 2-m RCC and the 1.3-m RC telescopes. Evidences of periodicity in the brightness variability of the star are not detected.
Variability with largest amplitude of FHO 28 is observed in 2012 July (2.49 mag in R-band). The measured colour indices V − I and V − R versus the stellar V magnitude during the period of our photometric observations are plotted in Figure 7. Irrespective of the large amplitude of variability, the substantial bluing effect is not seen on the figure. This means that the objects causing eclipses have a size significantly larger than the dust particles in the circumstellar environment of UXor variables. It can be supposed that in this case we observe eclipses from a combination of multiple bodies rotating in orbits around the star.
Figure 7. Relationship between V magnitude and the V − I and V − R colour indices of FHO 28 in the period 1997 June–2014 December.
3.4. FHO 29
The star FHO 29 (2MASS J20583974+4401328) is included in the list of YSO candidates by Guieu et al. (Reference Guieu, Rebull, Stauffer, Hillenbrand and Carpenter2009). The authors measured B = 18.288, V = 16.892, and I = 14.890 mag of the star. Rebull et al. (Reference Rebull2011) classify FHO 29 as a flat spectrum source. Findeisen et al. (Reference Findeisen, Hillenbrand, Ofek, Levitan, Sesar, Laher and Surace2013) presented R-band light curve of the star for the period 2011–2012 and described bursting events of the star.
The BVRI light curves of FHO 29 from our CCD observations in the period 2004–2014 are shown in Figure 8. The symbols used for the different telescopes are as in Figure 2. The results of our long-term multicolour CCD observations of the star are summarized in Table A4. The columns have the same contents as in Table A2.
Figure 8. CCD IRVB light curves of FHO 29 for the period 2004 November–2014 December.
The brightness of FHO 29 during the period of our observations vary in the range 14.29–17.47 mag for I-band, 15.28–18.12 mag for R-band, and 16.27–19.01 mag for V-band. The observed amplitudes are 3.18 mag for I-band, 2.84 mag for R-band, and 2.74 mag for V-band in the same period, because the limit of our photometric data the deep fading events of FHO 29 in B-bands are not registered.
It can be seen from Figure 8, that until the end of 2011 FHO 29 exhibits irregular variations, then in the beginning of 2012 it began to increase its brightness and in mid-2012 the brightness of the star began sharply to drop, reaching amplitudes 3.10 mag for I-band, 2.70 mag for R-band, and 2.60 mag for V-band in May 2012. Several sharp increases in brightness for periods of several days or weeks were observed in 2013. At the end of 2013, a gradual drop in brightness started following by a gradual rise by the end of 2014. We can confirm that the long-term light curve of FHO 29 is dominated by burst events. Evidences of periodicity in the brightness variability of the star are not registered. R-band images of FHO 29 at maximum (2010 June 10) and at minimum light (2013 May 2) are shown on Figure 9.
Figure 9. The star FHO 29 at maximum (2010 June 10, the left image) and at minimum light (2013 May 2, the right image). The frames were taken in R-band with Schmidt telescope of Rozhen NAO.
The measured colour indices V − I, V − R, and B − V versus the stellar V magnitude during the period of our observations are plotted in Figure 10. In contrast to other objects from our study, for FHO 29 we observe an increase of the colour indices against an increase in the brightness of the star. This relationship can be seen in Figure 8 also, the amplitude of the brightness in I-band is larger than the amplitudes in R- and V-bands, respectively. Such a reverse of the colour indices is in a conflict with the bursting nature of the star. On the other hand, the star cannot be classified as UXor, as well as it spends more time at a low light.
Figure 10. Relationship between V magnitude and the V − I, V − R, and B − V colour indices of FHO 29 in the period 2004 November–December 2014.
3.5. V1929 Cyg
The star V1929 Cygni was discovered and classified as a flare star by Rosino et al. (Reference Rosino, Tsvetkov and Tsvetkova1987). The authors reported a flare event on 1972 September 4 when the brightness of the star increased from 16.50 mag pg to 14.50 mag pg. The magnitudes and colours of V1929 Cyg in quiescence measured by Tsvetkov et al. (Reference Tsvetkov, Semkov, Tsvetkova and Hambaryan1996) are V = 15.24 mag, B − V = 0.92 mag, V − R = 0.64 mag, and V − I = 1.28 mag. The authors provide spectrum of V1929 Cyg and estimate its spectral type as dK2-dK5, with Hα in emission.
Laugalys et al. (Reference Laugalys, Straižys, Vrba, Boyle, Philip and Kazauskas2006) measured V = 15.111 mag and V − U = 3.337 mag for V1929 Cyg and determined its photometric spectral type as ‘K0V,e?’. From a spectrum taken on 2007 October 22 by Corbally, Straižys, & Laugalys (Reference Corbally, Straižys and Laugalys2009), the authors identify faint Hα emission line and OI, CaII and P9 lines. The spectral type is determined as G8e, but on the J − H/H − Ks diagram the star lies close to the K dwarf sequence. The authors suggest that the energy distribution of the star, constructed from Spitzer observations does not show any infrared emission and the authors conclude that the star seems to be a slightly reddened G dwarf with chromospheric activity. The distance to V1929 Cyg determined by Corbally et al. (Reference Corbally, Straižys and Laugalys2009) is 580 pc, i.e., close to the distance of the NGC 7000/IC 5070 complex.
The multicolour BVRI light curves of V1929 Cyg from our CCD observations are shown in Figure 11. The symbols used for the different telescopes are as in Figure 6. The results of our long-term photometric observations are summarised in Table A5. The columns have the same contents as in Table A2.
Figure 11. CCD IRVB light curves of V1929 for the period 2000 October –December 2014.
From the Figure 11 can be seen that during the period of our observations V1929 Cyg shows irregular variability in all bands, but flare events are not registered. The brightness of the star during the period 2000–2014 vary in the range of 13.61–13.98 mag for I-band, 14.17–14.62 mag for R-band, 14.77–15.27 mag for V-band, and 15.75–16.26 mag for B-band. The observed amplitudes are ΔI = 0.37 mag, ΔR = 0.45 mag, ΔV = 0.50 mag, and ΔB = 0.51 mag in the same period. Usually, such low amplitude variability is typical for low-mass WTTS.
The measured colour indices V − I, V − R, and B − V versus stellar V magnitude during the period of our CCD observations are plotted in Figure 12. The colour variations are typical of WTTS, stars with cool spots, whose variability is produced by rotation of the spotted surface.
Figure 12. Relationship between V magnitude and the V − I, V − R, and B − V colour indices of V1929 Cyg in the period 2000 October–2014 December.
We carried out a periodicity search using our data from 2012 April to 2014 December by persea Version 2.6 (written by G. Maciejewski on the ANOVA technique, Schwarzenberg-Cherny (Reference Schwarzenberg–Cherny1996)) and period04 (Lenz & Breger Reference Lenz and Breger2005) softwares. Our time-series analysis of the data indicates a 0.426257 ± 0.000306 day period and led to the ephemeris:
\begin{equation}
\text{JD} (\text{Max}) = 2455113.949113 + 0.426257 * E.
\end{equation}
False Alarm Probability estimation was done by randomly deleting about 10%–15% of the data for about 30 times and then retuning the period of determination. The period and starting age (T 0) determination remain stable, even with a subsample with 30% of the data removed.
Figure 13 exhibits the V-band folded light curve of V1929 Cyg according to the ephemeris (1). The data obtained in BRI-bands show the same shape on periodicity. The found period is stable during time interval of several years and it is typical rotational period of young low-mass star. The periodicity could be caused by rotation modulation of the dark spots on the stellar surface. Such rotation period is extremely short for TTS, but still compatible with the shortest rotation periods of others WTTS (Herbst et al. Reference Herbst, Eisloffel, Mundt, Scholz, Reipurth, Jewitt and Keil2007; Scholz et al. Reference Scholz, Irwin, Bouvier, Sipőcz, Hodgkin and Eislöffel2011).
Figure 13. V-band folded curve of V1929 Cyg.
4 CONCLUSION
We investigated the long-term photometric behaviour of five PMS stars located in the region of ‘Gulf of Mexico’. The stars FHO 26 and FHO 29 are likely CTTS showing large amplitude bursting events, while FHO 27 and FHO 28 have indications for variable extinction from the circumstellar environment. On the basis of the observed different shapes of the drops in the brightness, we assume that there is likely to exist a variety of obscuration reasons. V1929 Cyg seems to be WTTS with extremely short rotation period and flare events from UV Cet type.
We are continuing to collect photometric observations of the field of ‘Gulf of Mexico’. The long-term multicolour photometric observations of YSOs are very important for their exact classification. Further regular observations of the YSOs in the same field will be of a great importance and are encouraging.
ACKNOWLEDGEMENTS
The authors thank the Director of Skinakas Observatory Prof. I. Papamastorakis and Prof. I. Papadakis for the award of telescope time. The research has made use of the NASA’s Astrophysics Data System Abstract Service and the SIMBAD database, operated at CDS, Strasbourg, France. This study was partly supported by the European Social Fund and the Ministry of Education and Science of Bulgaria under the contract BG051PO001-3.3.06-0047.
APPENDIX. PHOTOMETRIC CCD OBSERVATIONS AND DATA OF THE STARS FROM OUR STUDY
Table A1. Photometric CCD observations and data of FHO 26 during the period 2000 October–2014 December.
Table A2. Photometric CCD observations and data of FHO 27 during the period 2000 October–2014 December.
Table A3. Photometric CCD observations and data of FHO 28 during the period 1997 June–2014 December.
Table A4. Photometric CCD observations and data of FHO 29 during the period 2004 November–2014 December.
Table A5. Photometric CCD observations and data of V1929 Cygni during the period 2010 October–2014 December.
