Gayane Kostandyan Byurakan Astrophysical Observatory Byurakan, Armenia [email protected]

PhD student Supervisor Kamo Gigoyan April, 2019 B.E.Markarian, Authors: V.A.Lipovetsky, J.A.Stepanian Years: 1965-1980 102/132/213 cm Byurakan Schmidt telescope, 1.5° Instruments: objective prism (1800 Å/mm at Hγ) Kodak IIA-F, IIa-F, 103a-F, II- Emulsions: F 3400-6900 Å with a sensitivity Spectral range: gap near 5300 Å

Field: 4.1° x 4.1° (plates: 16 x 16 cm) Scale: 96.8 "/mm Region of sky: δ≤ -15°, |b| > 15° 17,056 sq. degree (1139 fields, Total area: more than 1874 plates) Limiting magn: 17m-17.5m (≤18.5m) Main goal: selection of UV-excess galaxies

UV gal, Sy, QSO, BLL, LINER, Selected objects: SB, HII, radiogalaxies, etc. Number of objs: 1515 15 lists (1967-1981), 2 catalogs Publication: (Mazzarella & Balzano 1986, Markarian et al. 1989) First Byurakan Survey (FBS)

● The discovery of 1515 UV-excess (UVX) galaxies by Markarian and colleagues (later called Markarian galaxies) ● Spectral Classification of Seyfert Galaxies (Weedman &Khachikian 1971) ● First Definition of Starburst Galaxies (Weedman 1977) Since 2007 all the FBS spectral plates are digitized. DFBS is a joint project of the Byurakan Astrophysical Observatory (BAO), Cornell University (USA) and Universita di Roma “La Sapienza” (Italy).

DFBS database is publicly available http://byurakan.phys.uniroma1.it/ https:/ia2.inaf.it/dfbs “Revised Survey of Late-Type Stars” (LTSs K.Gigoyan, A. Mickayelian, MNRAS, v. 419, 2012, CDS Vizier catalogue at http:/vizier.u-strasbg.fr/viz-bin/Vizier?-source=III/266) Digitized FBS spectral plates

DFBS image for M –dwarf FBS DFBS image for FBS 0519+085 0148+071 (M2-M3-subclass). which is N-type (wedge-like spectra) AGB C star TiO 4584,4762,4954,5167,5500, 6200 and 6700 Å C2 4737,5165 and 5636 Å N-type C star spectra M- type star spectra (M 8-9)

CH-type spectra M-type star spectra M 5-6 They have quite distinctive spectral characteristics, and were first recognazed by their spectra by Angelo Secchi in the 1860s, a pioneering time in astronomical spectroscopy .

Angelo Secchi(1818-1878) - an Italian astronomer. He was Director of the Observatory at the Pontifical Gregorian University for 28 years. Secchi is known for pioneering an astronomical spectroscopy and valuable contribution to the field of Sun study. Special interest was the Sun. Angelo was one of the first scientists to state authoritatively that the Sun is a star. He also revised Struve′s catalog of double stars, compiling data for over 10000 binaries, and discovered three comets. Spectral Class - Modern Revised by Morgan-Keenan (MK) • C-R • C-N • C-H -> used to be R-peculiar • C-J • C-Hd • Proper motion • Enhanced C2(0,2) bandhead at λ 6191A that is less pronounced in spectra of C giant • Multiple bands of CaH molecule at λ 6382, 6750, 6903A • Anomalous NIR colors Late-type(N-type) stars

Exhibit strong depression of radiation in the violet part of the spectrum Early-type stars (CH, R) Northern Sky variability Survey(NSVS) “General Catalogue of Galactic Carbon stars” Mira-type variables ∆R > 1.5 mag

Catalina Sky Survey(CSS) “CSS catalogue of variable stars” Mira-type variables ∆V >2.5 mag

Phase dependence light curve analysis and variability type classification was peformed with help of Vstar Software(a multi-platform data visualization and analysis tool, available at http://www.aavso.org/). Phase dependence light curve of late-type C stars

FBS 0826+185

Early-type 72 Carbon FBS stars ▪ 63 stars as CH , ▪ 4 stars as R ▪ 5 stars as dC canditates

Late-type 54(N-type) Carbon FBS stars ▪ 9 stars as Mira-type variables ▪ 43 stars as Semi-Regular(SR) type variables ▪ 2 stars as Irregular(Irr) type variables • JHKs photometry from 2MASS catalog • IRAS • AKARI (at 9 and 18 μm) • WISE (at 3.4, 4.6, 12 and 22 μm) • Spitzer Two – color JHK diagram WISE W1-W2 vs. W3-W4 and W1-W2 vs. W1-W4 color-color plots(with errors bars) for all C stars. Crosses are early-type stars, filled squares are late N-type stars. 2MASS J-Ks vs. Ks-AKARI 9mag. and J-Ks vs. Ks-W4 color-color diagram for all 126 C stars . The reddest object is N-type star FBS 2213+421, which belongs to the cold post-AGB R Corone Borealis ( R CrB ) variables. IRAS – SPITZER spectroscopy

IRAS Low-Resolution Spectra (LRS) in wavelength range 7.7÷22.6 µm(Fig.a) and Spitzer/IRS spectra(Fig. b) in wavelength range 5÷38 µm for FBS1812+455 Spectral Energy Distribution - SED UU U CUM IR-Color and Mass-Loss Rates

log(Mtotal) = -7.668 + 0.7305(K-[12]) – 5.398x10ˉ²(K-[12])² + 1.343x10ˉ³(K-[12])³ where [12] is IRAS 12µm band magnitude defines as: [12] = 3.63 – 2.5xlog.F(12) where F(12) is the IRAS flux in Jansky at 12µm logM = (4.08±0.41)xlogP-(16.54±1.1) = 0.27

FBS+DFS Number 2MASSAssociation logM(K-[12]) logM(P)

FBS 0043+474 0046248.+4741330 -6.18 -6.19 FBS 0155+384 01580610+3839185 -7.00 -6.43 FBS 0158+095 02005614+0945356 -5.36 -5.38 FBS 0502+088 05050029+0856078 -6.00 -5.80 FBS 0729+269 07323273+2647156 -6.60 -6.60 FBS 1812+455 18132945+4531175 -5.13 -5.92 DFBS J064958.64+741610.1 06495846+7416107 -5.80 -6.08 DFBS J230835.19+403533.9 23082356+4035287 -6.06 -6.10 Summary

• All Digitized First Byurakan Survey (DFBS) spectral plates are analyzed with the help of standard image analysis software (FITSView and SAO Image ds9) on the base of present of the absorption bands of C 2 and TiO molecule in the low-resolution spectrum of the objects. • We revised, updated and generated the new version of the FBS LTS catalogue. The second version of the catalogue contains main available data for 1471 objects. • Large number of the FBS LTSs are completely new objects, which promise to expand the census of M giants and M dwarfs in the Solar vicinity. • Gaia DR2 important astrophysical parameters such as parallaxes, Gmag, T eff , radius and luminosities (in Solar units) are presented for all 1471 FBS LTS stars. • In combination with new Gaia DR2 data with the existing photometric and spectroscopic data, further studies are needed to clarify the nature of the FBS LTS, particularly the origin of the high radial velocity M- giants, N-type AGB C stars, and CH-type faint C stars at high Galactic latitudes and in Galactic Halo.