Satellites and central galaxies in SDSS: the influence of interactions on their properties

Mesa, Valeria; Alonso, Santiago; Coldwell, Georgina; Lambas, D. García; Castellón, J. L. Nilo

doi:10.1093/mnras/staa3720

Cited by 3 publications

(2 citation statements)

References 71 publications

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“…They are not necessarily absolutely constant stars, but may not exhibit significant radial velocity variation during the time-domain survey. can be used to understand galaxy formation and evolution (Gao et al 2015;Mesa et al 2021). As a fundamental property that can be measured directly from stellar spectra, radial velocity (RV) is the basic ingredient for many studies, such as study of the properties of a binary (Gao et al 2014;Tian et al 2018;Sana et al 2012Sana et al , 2013, Milky Way dynamics (Tian et al 2020), asteroseismology (Arentoft et al 2019) and even searching for black holes (Liu et al 2019).…”

Section: Introductionmentioning

confidence: 99%

The relative calibration of radial velocity for LAMOST medium resolution stellar spectra

Xiong

Zhang

Liu

et al. 2021

Res. Astron. Astrophys.

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The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) started a median-resolution spectroscopic (MRS, R ∼7500) survey since October 2018. The main scientific goals of MRS, including binary stars, pulsators and other variable stars, were launched with a time-domain spectroscopic survey. However, the systematic errors, including the bias induced from wavelength calibration and the systematic difference between different spectrographs, have to be carefully considered during radial velocity measurement. In this work, we provide a technique to correct the systematics in the wavelength calibration based on the relative radial velocity measurements from LAMOST MRS spectra. We show that, for the stars with multi-epoch spectra, the systematic bias which is induced from the exposures on different nights can be corrected well for LAMOST MRS in each spectrograph. In addition, the precision of radial velocity zero-point of multi-epoch time-domain observations reaches below 0.5 km s−1. As a by-product, we also give the constant star candidates**, which can be the secondary radial-velocity standard star candidates of LAMOST MRS time-domain surveys.

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Section: Introductionmentioning

confidence: 99%

The relative calibration of radial velocity for LAMOST medium resolution stellar spectra

Xiong

Zhang

Liu

et al. 2021

Res. Astron. Astrophys.

View full text Add to dashboard Cite

show abstract

“…Over the past years, the large spectroscopic surveys, such as RAVE (Steinmetz et al, 2006(Steinmetz et al, , 2020, SDSS/SEGUE (Yanny et al, 2009), LAMOST (Cui et al, 2012;Deng et al, 2012;Zhao et al, 2012;Luo et al, 2015), APOGEE (Majewski et al, 2017), GALAH (De Silva et al, 2015), Gaia (Gilmore et al, 2012;Katz et al, 2004;Cropper et al, 2018) have yielded a large number of stellar spectra to understand the galaxy formation and evolution (Gao et al, 2015;Mesa et al, 2021). As a fundamental property that can be measured directly from stellar spectra, radial velocity (RV) is the basic ingredient for many studies, such as the study on the properties of binary (Gao et al, 2014;Tian et al, 2018;Sana et al, 2012Sana et al, , 2013, Milky Way dynamics (Tian et al, 2020), asteroseismology (Arentoft et al, 2019), and even searching for the black holes (Liu et al, 2019).…”

Section: Introductionmentioning

confidence: 99%

The Relative Calibration of Radial Velocity for LAMOST Medium Resolution Stellar Spectra

Xiong,

Zhang,

Liu

et al. 2021

Preprint

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The Large Sky Area Multi-Object Fiber Spectroscopic Telescope (LAMOST) started medianresolution spectroscopic (MRS, R∼7500) survey since October 2018. The main scientific goals of MRS, including binary stars, pulsators, and other variable stars are launched with a time-domain spectroscopic survey.However, the systematic errors, including the bias induced from wavelength calibration and the systematic difference between different spectrographs have to be carefully considered during radial velocity measurement. In this work, we provide a technique to correct the systematics in the wavelength calibration based on the relative radial velocity measurements from LAMOST MRS spectra. We show that, for the stars with multi-epoch spectra, the systematic bias which is induced from the exposures of different nights can be well corrected for LAMOST MRS in each spectrograph. And the precision of radial velocity zero-point of multi-epoch timedomain observations reaches below 0.5 km s −1 . As a by-product, we also give the constant star candidates , which can be the secondary radial-velocity standard star candidates of LAMOST MRS time-domain surveys.

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The AMIGA sample of isolated galaxies

Sánchez-Alarcón¹,

Román²,

Knapen³

et al. 2023

A&A

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Context. In the standard cosmological model of galaxy evolution, mergers and interactions play a fundamental role in shaping galaxies. Galaxies that are currently isolated are thus interesting because they allow us to distinguish between internal and external processes that affect the galactic structure. However, current observational limits may obscure crucial information in the low-mass or low-brightness regime. Aims. We use optical imaging of a subsample of the AMIGA catalogue of isolated galaxies to explore the impact of different factors on the structure of these galaxies. In particular, we study the type of disc break as a function of the degree of isolation and the presence of interaction indicators such as tidal streams or plumes, which are only detectable in the ultra-low surface brightness regime. Methods. We present ultra-deep optical imaging in the r band of a sample of 25 low-redshift (z < 0.035) isolated galaxies. Through careful data processing and analysis techniques, the nominal surface brightness limits achieved are comparable to those to be obtained on the ten-year LSST coadds (μr,lim ≳ 29.5 mag arcsec−2 [3σ; 10″ × 10″]). We place special emphasis on preserving the low surface brightness features throughout the processing. Results. The extreme depth of our imaging allows us to study the interaction signatures of 20 galaxies since Galactic cirrus is a strong limiting factor in the characterisation of interactions for the remaining 5 of them. We detect previously unreported interaction features in 8 (40% ± 14%) galaxies in our sample. We identify 9 galaxies (36% ± 10%) with an exponential disc (Type I), 14 galaxies (56% ± 10%) with a down-bending (Type II) profile, and only 2 galaxies (8% ± 5%) with up-bending (Type III) profiles. Isolated galaxies have considerably more purely exponential discs and fewer up-bending surface brightness profiles than field or cluster galaxies. We find clear minor merger activity in some of the galaxies with single exponential or down-bending profiles, and both of the galaxies with up-bending profiles show signatures of a past interaction. Conclusions. We show the importance of ultra-deep optical imaging in revealing faint external features in galaxies that indicate a probable history of interaction. We confirm that up-bending profiles are likely produced by major mergers, while down-bending profiles are probably formed by a threshold in star formation. Unperturbed galaxies that slowly evolve with a low star formation rate could induce the high rate of Type I discs in isolated galaxies.

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Satellites and central galaxies in SDSS: the influence of interactions on their properties

Cited by 3 publications

References 71 publications

The relative calibration of radial velocity for LAMOST medium resolution stellar spectra

The relative calibration of radial velocity for LAMOST medium resolution stellar spectra

The Relative Calibration of Radial Velocity for LAMOST Medium Resolution Stellar Spectra

The AMIGA sample of isolated galaxies

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