Radio stars observed in the LAMOST spectral survey

Radio stars have attracted astronomers' attention for several decades. To better understand the physics behind stellar radio emissions, it is important to study their optical behaviors. The LAMOST survey provides a large database for researching stellar spectroscopic properties of radio stars. In this work, we concentrate on their spectroscopic properties and infer physical properties from their spectra,such as stellar activity and variability. We mined big data from the LAMOST spectral survey Data Release 2(DR2), published on 2016 June 30, by cross-matching them with radio stars from FIRST and other surveys. We obtained 783 good stellar spectra with high signal to noise ratio for 659 stars. The criteria for selection were positional coincidence within 1.5′′and LAMOST objects classified as stars.We calculated the equivalent widths(EWs) of the Ca II HK, Hδ, Hγ, Hβ, Hα and Ca II IRT lines by integrating the line profiles. Using the EWs of the Hα line, we detected 147 active stellar spectra of 89 objects having emissions above the Hα continuum. There were also 36 objects with repeated spectra,28 of which showed chromospheric activity variability. Furthermore, we found 14 radio stars emitting noticeably in the Ca II IRT lines. The low value of the EW8542/EW8498 ratio for these 14 radio stars possibly alludes to chromospheric plage regions.     

Long-term BV RI photometric light curves of 15 PMS stars in the star-forming region IC 5070

This paper reports results from the multicolor photometric observations of 15 pre-main sequence stars collected in the period September 2010-October 2017. The stars from our study are located in the star-forming HII region IC 5070. These objects were previously detected as either emission line stars, flare stars, T Tauri variables or Herbig Ae/Be stars. Photometric observations, especially concerning the long-term behavior of the objects, are missing in the literature. We present the first photometric monitoring for all stars from our study. The analysis of the obtained BV RI photometric data allows us to draw the conclusion that all investigated objects are variable stars. In the case of LkHα 146,we identified previously unknown periodicity in its photometric variability.     

Line profile studies of hydrodynamical models of cometary compact H II regions

We simulate the evolution of cometary H II regions based on several champagne flow models and bow shock models, and calculate the profiles of the [Ne II]fine-structure line at 12.81 μm, the H30α recombination line and the [Ne III] finestructure line at 15.55 μm for these models at different inclinations of 0?, 30?and 60?.We find that the profiles in the bow shock models are generally different from those in the champagne flow models, but the profiles in the bow shock models with lower stellar velocity(≤ 5 km s-1) are similar to those in the champagne flow models. In champagne flow models, both the velocity of peak flux and the flux weighted central velocities of all three lines point outward from molecular clouds. In bow shock models, the directions of these velocities depend on the speed of stars. The central velocities of these lines are consistent with the stellar motion in the high stellar speed cases, but they are opposite directions from the stellar motion in the low speed cases.We notice that the line profiles from the slit along the symmetrical axis of the projected 2D image of these models are useful for distinguishing bow shock models from champagne flow models. It is also confirmed by the calculation that the flux weighted central velocity and the line luminosity of the [Ne III] line can be estimated from the[Ne II] line and the H30α line.     

Be星光谱和近红外光度观测

Equivalent widths (EW) of Hα emission lines and JHK magnitudes for 24 Be Stars were measured. Spectroscopic and near infrared photometric Observations were made with 216 cm telescope and 126 cm telescope separately at Beijing Astronomical Observatory in the autumn of 1992. Some additional apectra were obtained with 100 cm telescope at Yunnan Astronomical Observatory in January 1993.As a preliminary analysis of the data, the correlation between EW of Hαand colour index J-K of Be Stars was investigated. The EW as a function of J-K were plotted. It is shown that the EW of Hα emission line is proportional to J-K quite well for Be Stars we observed, except two stars: KX And and LSI 61 °303, of which the infrared excess are too large, ΔEW /Δ(J-K) is equal to 100 A / magnitude, this correlation indicates that both infrared excess and Hα emission originate in a commom region of envelope around Be stars.     

Hα profile variations in the spectrum of the supergiant HD14134

Variations of the Hα line in the spectra of the star HD14134 are investigated using observations carried out in 2013–2014 and in 2016 with the 2-m telescope at Shamakhy Astrophysical Observatory.In the spectra of this star,the absorption and emission components of Hα are found to disappear and an inverse P Cyg profile of Hα is seen on some observational epochs.Our observations showed that when the Hα line disappeared or an inversion of the P-Cyg-type profile is observed in the spectra,the Hβ line is redshifted.When these events appeared,no synchronous variabilities were observed in the spectral parameters of other spectral lines formed in deeper atmospheric layers.In addition,the structures of Hα,CII(6578.05 ,6582.88 ),SiII(6347.1 ,6371.36 ) and Hβ lines are variable on a timescale of hours,but we did not detect significant variations in the other photospheric lines,as well as in the HeI(5875.72 ) line.It is suggested that observational evidence for the non-stationary atmosphere of HD14134 can be associated in part with non-spherical stellar wind.     

Spectroscopic study of Be-shell stars: 4 Her and 88 Her

We present an optical spectroscopic study based on 41 spectra of 4 Her and 32 spectra of 88 Her,obtained over a period of 6 months.We estimate the rotational velocity of these stars from Hel lines in the blue spectral region(4000-4500 ?).We find that these stars are likely to be rotating at a fractional critical rotation of~0.80.We measure the average I_p/I_c ratio to quantify the strength of the Hα line and obtain1.63 for 4 Her and 2.06 for 88 Her.The radius of the Ha emission region is estimated to be R_d/R_*~5.0,assuming a Keplerian disk.These stars are thus found to be fast rotators with a relatively small Ha emission region.We detect V/R variation of the Ha spectral line during the observed period.We re-estimate the periods for both stars and obtain a period of ~46 d and its harmonic of 23.095 d for 4 Her,and a period of~86 d for 88 Her.As these two cases are shell stars with binaries and have low Ha EW with the emission region closer to the central star,the V/R variation and a change in period may be an effect of the binary on the circumstellar disk.     

A catalogue of Hα emission-line point sources in the vicinity fields of M31 and M33 from the LAMOST survey

We present a catalogue of 3305 Hα emission-line point sources observed with the Large Sky Area Multi-Object Fiber Spectroscopic Telescope(LAMOST) in the vicinity fields of M31 and M33 during September 2011 and January 2016.The catalogue contains 1487 emission-line stars,532 emission-line nebulae including 377 likely planetary nebulae(PNe),83 H Ⅱ region candidates and 20 possible supernova remnants(SNRs) and 1286 unknown objects.Among them,24 PN candidates,19 H Ⅱ region candidates,10 SNR candidates and one symbiotic star candidate are new discoveries.Radial velocities and fluxes estimated from the Hα line and those quantities of seven other major emission lines including Hβ,[O Ⅲ] A4959,[O Ⅲ] A5007,[N Ⅱ] A6548,[N Ⅱ] A6583,[S Ⅱ] A6717 and [S Ⅱ] A6731 lines of all the catalogued sources yielded from the LAMOST spectra are also presented in our catalogue.Our catalogue is an ideal starting point to study the chemistry properties and kinematics of M 31 and M 33.     

Optical/IR studies of Be stars in NGC 6834 with emphasis on two specific stars

We present optical and infrared photometric and spectroscopic studies of two Be stars in the 70–80-Myr-old open cluster NGC 6834. NGC 6834(1) has been reported as a binary from speckle interferometric studies whereas NGC 6834(2) may possibly be a γ Cas-like variable. Infrared photometry and spectroscopy from the United Kingdom Infrared Telescope(UKIRT), and optical data from various facilities are combined with archival data to understand the nature of these candidates.High signal-to-noise near-IR spectra obtained from UKIRT have enabled us to study the optical depth effects in the hydrogen emission lines of these stars. We have explored the spectral classification scheme based on the intensity of emission lines in the H and K bands and contrasted it with the conventional classification based on the intensity of hydrogen and helium absorption lines. This work also presents hitherto unavailable UBV CCD photometry of NGC 6834, from which the evolutionary state of the Be stars is identified.     

Stellar population analysis on the stacked spectra of double-peaked emission-line galaxies

Double-peaked emission-line galaxies have long been perceived as objects related to merging galaxies or other phenomena with disturbed dynamical activities, such as outflows and disk rotation. In order to find the connection between the unique activities happening in these objects and their stellar population physics, we study the stellar populations of the stacked spectra drawn from double-peaked emission-line galaxies in the Large Sky Area Multi-Object Fiber Spectroscopic Telescope(LAMOST) Data Release 4(DR4) and the Sloan Digital Sky Survey(SDSS) Data Release 7(DR7) databases. We group the selected double-peaked emission-line objects into 10 different types of pairs based on the Baldwin-Phillips-Terlevich(BPT) diagnosis for each pair of blueshifted and redshifted components, and then stack the spectra of each group for analysis. The software STARLIGHT is employed to fit each stacked spectrum, and the contributions of stars at different ages and metallicities are quantified for subsequent comparative study and analysis. To highlight the commonality and uniqueness in these double-peaked emitting objects, we compare the population synthesis results of the stacked spectra of double-peaked emission-line galaxies with those of their counterpart reference samples displaying single-peaked emission features. The reference samples are also selected from the LAMOST DR4 and SDSS DR7 databases. From the comparison results,we confirm the strong correlations between stellar populations and their spectral classes, and find that the double-peaked emitting phenomenon is more likely to occur in an ‘older' stellar environment and the subgroups hosting different BPT components will show an obvious heterogeneous star formation history.     

Cataclysmic variables based on the stellar spectral survey LAMOST DR3

Big data in the form of stellar spectra from the spectroscopic survey associated with the Large Sky Area Multi-object Fiber Spectroscopic Telescope(LAMOST) are important for studying properties of cataclysmic variables(CVs). By cross matching the catalogs of CVs compiled with LAMOST DR3,acquired from October 2011 to July 2015, we obtained the first spectroscopic catalog for CVs observed by LAMOST with high signal to noise ratio, above 8. By integrating line profiles, their equivalent widths(EWs) of the Hα, Hβ, Hγ and Hδ, as well as He I 5876 and 6678 A? lines, were calculated. There were74 stellar spectra from 48 known CVs and three spectra from three new CV candidates. At the same time, we also collected their previously published EWs. Thirty-three objects had repeated spectra and30 stars showed spectral variability in the Hα line. Moreover, we carried out photometric follow-up studies for five CVs(UU Aqr, TT Tri, PX And, BP Lyn and RW Tri). We obtained nine new light curves and revised their linear ephemerides. For RW Tri, there is a possible oscillation with an amplitude of0.0031(2) days and a period of 47.6±0.4 years, which might be caused by a third body(brown dwarf)or magnetic activity cycle.     

Optical Spectroscopy of Classical Be Stars in Old Open Clusters

We performed the optical spectroscopy of 16 classical Be stars in 11 open clusters older than 100 Myr. Ours is the first spectroscopic study of classical Be stars in open clusters older than 100 Myr. We found that the Hα emission strength of most of the stars is less than 40 ?, in agreement with previous studies. Our analysis further suggests that one of the stars, [KW97] 35–12, might be a weak Hα emitter in nature, showing Hα equivalent width of-0.5 ?.Interestingly, we also found that the newly...     

Variability of emission lines in the optical spectra of the Herbig Be binary system HD 200775

In our previous papers we have improved the value of the orbital period of the binary Herbig Be star HD 200775 and showed that the [O I] and Si II 6347 and 6371 ?A emission lines displayed variations which correlate with the orbital period. In this paper we provide evidences that other broad emission lines of metals in the spectra of HD 200775 also exhibit variability, which is probably related to the orbital cycle of the binary. Analysis was performed based on the high-resolution spectral data collected over a time span of 6 years at the Kourovka Astronomical Observatory of the Ural Federal University(Russia) and the Three College Observatory of the University of North Carolina at Greensboro(USA) as well as archival spectral data compiled since 1994. We report new data points in the radial velocity curve of the He I 5876 ?A line near the extremal values of the radial velocity.     

On the reality of broad iron L lines from the narrow line Seyfert 1 galaxies 1H0707–495 and IRAS 13224–3809

We performed time resolved spectroscopy of 1H0707–495 and IRAS 13224–3809 using long XMM-Newton observations. These are strongly variable narrow line Seyfert 1 galaxies and show broad features around 1 ke V that have been interpreted as relativistically broad Fe Lα lines. Such features are not clearly observed in other active galactic nuclei despite sometimes having high iron abundance required by the best fitted blurred reflection models. Given the importance of these lines, we explore whether the rapid variability of spectral parameters may introduce broad bumps/dips artificially in the time averaged spectrum, which may then be mistaken as broadened lines. We tested this hypothesis by performing time resolved spectroscopy using long(100 ks) XMM-Newton observations and by dividing them into segments with typical exposures of a few ks. We extracted spectra from each such segment and modeled them using a two component phenomenological model consisting of a power law to represent the hard component and a black body to represent the soft emission. As expected, both the sources showed variations in the spectral parameters. Using these variation trends, we simulated model spectra for each segment and then co-added to get a combined simulated spectrum. In the simulated spectra, we found no broad features below 1 ke V and in particular no deviation near 0.9 ke V as seen in the real averaged spectra. This implies that the broad Fe Lα line that is seen in the spectra of these sources is not an artifact of the variation of spectral components and, hence, provides evidence that the line is indeed genuine.     

Relation between Starlight and Nebular Emission Lines of Star-Forming Galaxies

We present an exercise that intends to establish a relationship between the strength of nebular emission lines and optical stellar features in the spectrum of a galaxy. After accurately subtracting the stellar continuum and the underlying stellar absorption, we made reliable measurements of the emission lines of all the galaxies in the Sloan Digital Sky Survey Data Release 2 (SDSS DR2). More than 4000 star-forming galaxies with high S/N ratio of both the stellar spectrum and the emission lines are selected. These galaxy spectra are fitted with the 10 PCs of Yip et al., after all the emission line regions have been filtered out. We find that the flux of hydrogen Balmer emission lines, Hα and Hβ can be well recovered from the PCs, while the metal lines are not well reproduced. The fluxes of Hα and Hβ measured from the PC-reconstructed spectra and from the observed spectra agree well with an rms scatter of only - 0.1 dex. This result suggests that, with moderate spectral resolution and S/N ratio, the optical stellar spectrum of a galaxy can serve as an indicator of star formation rate.     

Optical flare events on the RS Canum Venaticorum star UX Arietis

Based on long-term high-resolution spectroscopic observations obtained during five observing runs from 2001 to 2004,we study optical flare events and chromospheric activity variability of the very active RS CVn star UX Ari.By means of the spectral subtraction technique,several optical chromospheric activity indicators(including the He I D_3,Na I D_1,D_2 doublet,Hα and Ca II IRT lines) covered in our echelle spectra were analyzed.Four large optical flare events were detected on UX Ari during our observations,which show prominent He I D_3 line emission together with great enhancement in emission of the Hα and Ca II IRT lines and strong filled-in or emission reversal features in the Na I D_1,D_2 doublet lines.The newly detected flares are much more energetic than previous discoveries,especially for the flare identified during the 2002 December observing run.Optical flare events on UX Ari are more likely to be observed around two quadratures of the system,except for our optical flares detected during the 2004 November observing run.Moreover,we have found rotational modulation of chromospheric activity in the Hα and Ca II IRT lines,which suggests the presence of chromospherically active longitudes over the surface of UX Ari.The change in chromospherically active longitudes among our observing runs,as well as the variation in chromospheric activity level from 2001 to 2004,indicates a long-term evolution of active regions.     

Measurements of the Ca II infrared triplet lines of young stellar objects

Equivalent widths and line widths of Ca II infrared triplet emission lines were measured in the high-resolution optical spectra of 39 young stellar objects.We found that the equivalent widths of the emission lines decrease with stellar evolution.It has often been claimed that strong chromospheric activity is generated by a dynamo process caused by fast rotation of the photosphere.However,we found no clear correlation between the strength of the Ca II lines and the stellar rotation velocity.Instead,we found that the objects with high mass accretion rates had stronger Ca II emission lines.This correlation supports the turbulent chromosphere model or the magnetic accretion theory for classical T Tauri stars.We also noticed that the equivalent widths of Ca II lines in transitional disk objects are one-tenth of those in classical T Tauri stars,even if the masses of the circumstellar disks are comparable.     

Synthetic analysis of a two-ribbon microflare

High-resolution Stokes spectral data of Hα,Ca II 8542 ,and Fe I 6302.5  lines for a two-ribbon microflare (TRMF) were simultaneously obtained by the THEMIS telescope on 2002 September 5.We derive the intensity,velocity,and longitudinal magnetic field maps.The hard X-ray emission observed by RHESSI provides evidence of nonthermal particle acceleration in the TRMF.Using Hα and Ca II 8542  line profiles and a non-LTE calculation,we obtain semi-empirical atmospheric models for the two brightest kernels of th...     

Photometry and spectroscopy of Ⅱ Peg,IM Peg and UX Ari

V band photometry of three RS CVn stars, II Peg, IM Peg and UX Ari, is carried out to study the physical properties of these variables. We verified the significant and regular optical photometric variability to be present in all three stars. The strong photometric variability and emission of Hα and Ca II H K using high resolution optical spectroscopy with the Hanle Echelle Spectrograph(HESP),which operates in conjunction with the Himalayan Chandra Telescope, verify the strong chromospheric activity which is present in RS CVn stars. The photometric studies of II Peg, UX Ari and IM Peg were subjected to light curve analysis for spot parameters using a two-starspot model.     

Chromospheric activity on the late-type star V1355 Ori using Lijiang 1.8-m and 2.4-m telescopes

We obtained new high-resolution spectra using the Lijiang 1.8-m and 2.4-m telescopes to investigate the chromospheric activities of VI355 Ori as indicated in the behaviors of Ca Ⅱ HK,Hδ,Hγ,Hβ,Na Ⅰ D_1,D_2,Hα and Ca Ⅱ infrared triplet(IRT) lines.The observed spectra show obvious emissions above the continuum in Ca II HK lines,absorptions in the Hδ,Hγ,Hβ and Na Ⅰ D_1,D_2 lines,variable behavior(filled-in absorption,partial emission with a core absorption component or emission above the continuum)in the Hα line,and weak self-reversal emissions in the strong filled-in absorptions of the Ca Ⅱ IRT lines.We used a spectral subtraction technique to analyze our data.The results show no excess emission in the Hδ and Hγ lines,very weak excess emissions in the Na Ⅰ D_1,D_2 lines,excess emission in the Hβ line,clear excess emission in the Hα line,and excess emissions in the Ca Ⅱ IRT lines.The value of the ratio of EW_(8542)/EW_(8498) is in the range 0.9 to 1.7,which implies that chromospheric activity might have been caused by plage events.The value of the ratio E_(Hα)/E_(Hβ) is above 3,indicating that the Balmer lines would arise from prominence-like material.We also found time variations in light curves associated with equivalent widths of chromospheric activity lines in the Na Ⅰ D_1,D_2,Ca Ⅱ IRT and Hα lines in particular.These phenomena can be explained by plage events,which are consistent with the behavior of chromospheric activity indicators.     

X-ray activity from different types of stars

X-ray emission is an important indicator of stellar activity. In this paper, we study stellar Xray activity using the XMM-Newton and LAMOST data for different types of stars. We provide a sample including 1259 X-ray-emitting stars, of which 1090 have accurate stellar parameter estimations. Our sample size is much larger than those used in previous works. We find a bimodal distribution of the X-ray to optical flux ratio(log(fX/fV)) for G and K stars. We interpret that this bimodality is due to two subpopulations with different coronal heating rates. Furthermore, using the full widths at half maxima calculated from Hα and Hβ lines, we show that these stars in the inactive peaks have smaller rotational velocities. This is consistent with the magnetic dynamo theory that presumes stars with low rotational velocities have low levels of stellar activity. We also examine the correlation between log(fX/fV) and luminosity of the excess emission in the Hα line, and find a tight relation between the coronal and chromospheric activity indicators.