UGC 1378 – a Milky Way sized galaxy embedded in a giant low surface brightness disc

Saburova, Anna S.; Chilingarian, Igor; Kasparova, Anastasia V.; Katkov, Ivan; Fabricant, Daniel G.; Уклеин, Р. И.

doi:10.1093/mnras/stz2434

Cited by 13 publications

(9 citation statements)

References 81 publications

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“…Despite their low central surface brightness they are sometimes as massive as many "regular" galaxies (see Figure 3 of Sprayberry et al 1995). The origin of giant LSBs has been much debated with many propositions, e.g., face-on collisions (Mapelli & Moore 2008), cooling gas during a merger (Zhu et al 2018;Saburova et al 2018), large initial angular momentum (Boissier et al 2003;Amorisco & Loeb 2016), accretion from cosmic filaments (Saburova et al 2019). Few spectroscopic studies were possible in giant LSBs (e.g., Saburova et al 2019), while they can bring important information to distinguish between these possibilities.…”

Section: Introductionmentioning

confidence: 99%

First spectroscopic study of ionised gas emission lines in the extreme low surface brightness galaxy Malin 1

Junais

Boissier

Épinat

et al. 2020

A&A

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Context. Malin 1 is the largest known low surface brightness (LSB) galaxy, the archetype of so-called giant LSBs. The structure and the origin of such galaxies are still poorly understood, especially due to the lack of high-resolution kinematics and spectroscopic data. Aims. We use emission lines from spectroscopic observations of Malin 1 aiming to bring new constraints on the internal dynamics and star formation history of Malin 1. Methods. We have extracted a total of 16 spectra from different regions of Malin 1 and calculated the rotational velocities of these regions from the wavelength shifts and star formation rates from the observed Hα emission line fluxes. We compare our data with existing data and models for Malin 1. Results. For the first time we present the inner rotation curve of Malin 1, characterized in the radial range r < 10 kpc by a steep rise in the rotational velocity up to at least ∼350 km s −1 (with a large dispersion), which had not been observed previously. We use these data to study a suite of new mass models for Malin 1. We show that in the inner regions dynamics may be dominated by the stars (although none of our models can explain the highest velocities measured) but that at large radii a massive dark matter halo remains necessary. The Hα fluxes derived star formation rates are consistent with an early-type disk for the inner region, and with the level found in extended UV galaxies for the outer parts of the giant disk of Malin 1. We also find signs of high metallicity but low dust content for the inner regions.

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Section: Introductionmentioning

confidence: 99%

First spectroscopic study of ionised gas emission lines in the extreme low surface brightness galaxy Malin 1

Junais

Boissier

Épinat

et al. 2020

A&A

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“…We add the sample of Coma UDGs (van Dokkum et al 2015, pink dimonds), low redshift galaxies (Trujillo et al 2020, small blue dots) and the sample in this work (red filled circles). We also show the results of giant LSBGs such as Marlin 1 (Galaz et al 2015), Marlin 2 (Kasparova et al 2014), UGC 1922(Saburova et al 2018, UGC 1378 (Saburova et al 2019) in open blue stars. We show the division line of the compact stellar system (thick line denoted by 100 pc), And the position of the stellar system with 1kpc, 10 kpc size.…”

Section: Stellar Mass Build Up Of the Lsbgmentioning

confidence: 89%

“…The current star formation in the LSBGs would build stars at a larger radius (Fig. 4), thus the LSBGs would evolve into an extended disk galaxy with higher stellar mass, such as the giant LSBGs such as Marlin 1 (Galaz et al 2015), Marlin 2 (Kasparova et al 2014), UGC 1922(Saburova et al 2018, UGC 1378 (Saburova et al 2019) in Fig. 7.…”

Section: Stellar Mass Build Up Of the Lsbgmentioning

confidence: 99%

UV and NIR size of the HI selected low surface brightness galaxies

Cheng,

Du,

et al. 2020

Preprint

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How does the low surface brightness galaxies (LSBGs) form stars and assemble the stellar mass is one of the most important questions to understand the LSBG population. We select a sample of 381 HI bright LSBGs with both Far Ultraviolet (FUV) and Near Infrared (NIR) observation to investigate the star formation rate (SFR) and stellar mass scales, and the growth mode. We measure the UV and NIR radius of our sample, which represent the star-forming and stellar mass distribution scales. We also compare the UV and H band radius-stellar mass relation with the archive data, to identify the SFR and stellar mass structure difference between the LSBG population and other galaxies. Since galaxy HI mass has a tight correlation with the HI radius, we can also compare the HI and UV radii to understand the distribution of the HI gas and star formation activities. Our results show that most of the HI selected LSBGs have extended star formation structure. The stellar mass distribution of LSBGs may have a similar structure as the disk galaxies at the same stellar mass bins, while the star-forming activity of LSBGs happens at a larger radius than the high surface density galaxies, which may help to select the LSBG sample from the wide-field deep u band image survey. The HI also distributed at a larger radius, implying a steeper (or no) Kennicutt-Schmidt relation for LSBGs.

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“…2, we show images of some represen- [197]. (center) UGC 1378 [198] a giant galaxy with a central high surface brightness disc surrounded by an extended LSB disc. (right)…”

Section: Structural Properties Of Lsb Galaxies 4659mentioning

confidence: 99%

“…Peculiar LSBs (left) the barred LSB galaxy UM163 from[197]. (center) UGC 1378[198] a giant galaxy with a central high surface brightness disc surrounded by an extended LSB disc. (right) The giant LSB galaxy Malin 1 from[199].…”

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confidence: 99%

Fundamental Properties of the Dark and the Luminous Matter from the Low Surface Brightness Discs

Salucci

Paolo

2021

Universe

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Dark matter (DM) is one of the biggest mystery in the Universe. In this review, we start reporting the evidences for this elusive component and discussing about the proposed particle candidates and scenarios for such phenomenon. Then, we focus on recent results obtained for rotating disc galaxies, in particular for low surface brightness (LSB) galaxies. The main observational properties related to the baryonic matter in LSBs, investigated over the last decades, are briefly recalled. Next, these galaxies are analyzed by means of the mass modelling of their rotation curves both individual and stacked. The latter analysis, via the universal rotation curve (URC) method, results really powerful in giving a global or universal description of the properties of these objects. We report the presence in LSBs of scaling relations among their structural properties that result comparable with those found in galaxies of different morphologies. All this confirms, in disc systems, the existence of a strong entanglement between the luminous matter (LM) and the dark matter (DM). Moreover, we report how in LSBs the tight relationship between their radial gravitational accelerations g and their baryonic components gb results to depend also on the stellar disk length scale and the radius at which the two accelerations have been measured. LSB galaxies strongly challenge the ΛCDM scenario with the relative collisionless dark particle and, alongside with the non-detection of the latter, contribute to guide us towards a new scenario for the DM phenomenon.

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UGC 1378 – a Milky Way sized galaxy embedded in a giant low surface brightness disc

Cited by 13 publications

References 81 publications

First spectroscopic study of ionised gas emission lines in the extreme low surface brightness galaxy Malin 1

First spectroscopic study of ionised gas emission lines in the extreme low surface brightness galaxy Malin 1

UV and NIR size of the HI selected low surface brightness galaxies

Fundamental Properties of the Dark and the Luminous Matter from the Low Surface Brightness Discs

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