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Dwarf Galaxy Discoveries from the KMTNet Supernova Program I. The NGC 2784 Galaxy Group
Astrophysics of Galaxies · Submitted 24 Aug 2017
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We interpret the baseline density level to represent the background contamination and so estimate that 22 of the 31 new candidates are dwarf members of the group.
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The abstract, sentence by sentence
We present $BVI$ surface photometry of 31 dwarf galaxy candidates discovered in a deep image stack from the KMTNet Supernova Program of $\sim$ 30 square degrees centered on the nearby NGC 2784 galaxy group. Our final images have a 3$\sigma$ surface brightness detection limit of $\mu_V\approx 28.5$ mag arcsec$^{-2}$. The faintest central surface brightness that we measure is $\mu_{0,V} = 26.1$ mag arcsec$^{-2}$. If these candidates are at the distance of NGC 2784, then they have absolute magnitudes greater than $M_V = -9.5$ mag and effective radii larger than 170 pc. Their radial number density decreases exponentially with distance from the center of NGC 2784 until it flattens beyond a radius of 0.5 Mpc. We interpret the baseline density level to represent the background contamination and so estimate that 22 of the 31 new candidates are dwarf members of the group. The candidate's average color, $\langle (B-V)_0\rangle\approx 0.7$, and Sersic structural parameters are consistent with those parameters for the dwarf populations of other groups. We find that the central population of dwarfs is redder and brighter than the rest of the population. The measured faint end slope of the luminosity function, $\alpha\approx-1.33$, is steeper than that of the Local Group but consistent with published results for other groups. Such comparisons are complicated by systematic differences among different studies, but will be simpler when the KMTNet survey, which will provide homogenous data for 15 to 20 groups, is completed.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present $BVI$ surface photometry of 31 dwarf galaxy candidates discovered in a deep image stack from the KMTNet Supernova Program of $\sim$ 30 square degrees centered on the nearby NGC 2784 galaxy group. | contribution 1.00 | 0.97 | 0.10 | asserted 1.00 |
| s1 | Our final images have a 3$\sigma$ surface brightness detection limit of $\mu_V\approx 28.5$ mag arcsec$^{-2}$. | result 0.66 | 0.95 | 0.03 | asserted 1.00 |
| s2 | The faintest central surface brightness that we measure is $\mu_{0,V} = 26.1$ mag arcsec$^{-2}$. | result 1.00 | 0.97 | 0.04 | asserted 1.00 |
| s3 | If these candidates are at the distance of NGC 2784, then they have absolute magnitudes greater than $M_V = -9.5$ mag and effective radii larger than 170 pc. | result 0.96 | 0.75 | 0.08 | hedged possibility 0.79 |
| s4 | Their radial number density decreases exponentially with distance from the center of NGC 2784 until it flattens beyond a radius of 0.5 Mpc. | result 1.00 | 0.93 | 0.10 | asserted 1.00 |
| s5 | We interpret the baseline density level to represent the background contamination and so estimate that 22 of the 31 new candidates are dwarf members of the group. | interpretation 0.85 | 0.95 | 0.39 | asserted 0.80 |
| s6 | The candidate's average color, $\langle (B-V)_0\rangle\approx 0.7$, and Sersic structural parameters are consistent with those parameters for the dwarf populations of other groups. | result 0.85 | 0.87 | 0.07 | hedged possibility 0.78 |
| s7 | We find that the central population of dwarfs is redder and brighter than the rest of the population. | result 1.00 | 0.97 | 0.10 | asserted 1.00 |
| s8 | The measured faint end slope of the luminosity function, $\alpha\approx-1.33$, is steeper than that of the Local Group but consistent with published results for other groups. | result 0.99 | 0.96 | 0.11 | asserted 0.99 |
| s9 | Such comparisons are complicated by systematic differences among different studies, but will be simpler when the KMTNet survey, which will provide homogenous data for 15 to 20 groups, is completed. | future work 0.81 | 0.16 | 0.04 | asserted 0.59 |
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The paper
Original abstract
We present $BVI$ surface photometry of 31 dwarf galaxy candidates discovered in a deep image stack from the KMTNet Supernova Program of $\sim$ 30 square degrees centered on the nearby NGC 2784 galaxy group. Our final images have a 3$\sigma$ surface brightness detection limit of $\mu_V\approx 28.5$ mag arcsec$^{-2}$. The faintest central surface brightness that we measure is $\mu_{0,V} = 26.1$ mag arcsec$^{-2}$. If these candidates are at the distance of NGC 2784, then they have absolute magnitudes greater than $M_V = -9.5$ mag and effective radii larger than 170 pc. Their radial number density decreases exponentially with distance from the center of NGC 2784 until it flattens beyond a radius of 0.5 Mpc. We interpret the baseline density level to represent the background contamination and so estimate that 22 of the 31 new candidates are dwarf members of the group. The candidate's average color, $\langle (B-V)_0\rangle\approx 0.7$, and Sersic structural parameters are consistent with those parameters for the dwarf populations of other groups. We find that the central population of dwarfs is redder and brighter than the rest of the population. The measured faint end slope of the luminosity function, $\alpha\approx-1.33$, is steeper than that of the Local Group but consistent with published results for other groups. Such comparisons are complicated by systematic differences among different studies, but will be simpler when the KMTNet survey, which will provide homogenous data for 15 to 20 groups, is completed.
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How the literature uses it
2 arXiv papers cite this in 3 sentences
Papers citing it · 1 sentence without a confident label
Uses its method or tool 1 paper
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Point-spread function photometry was performed using the DAOPHOT-II package [ref] on the KSP images, and the photometric standardization was made by comparing the brightness of with those of multiple nearby standard stars from the AAVSO Photometric All Sky Survey (APASS) database on the same images.[https://www.aavso.org/apass] This standardization method of KMTNet images requires a $B$-band color correction of $Δ$$m_B$ = $m_B - m_B'$ $≃$ 0.27 $(m_B-m_V)$ + offset, where $m_B$ and $m_B'$ are color-corrected $B$-band magnitudes in the standard Johnson system and uncorrected KTMNet $B$-band magnitudes, respectively [ref] .
A New WZ Sagittae-type Dwarf Nova KSP-OT-202104a Near the Period Minimum from the KMTNet Supernova Program · Observations and Discovery · 0.96
What it cites
Uses data or values from 1 paper
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To obtain the comparison LF's, we use photometry from the literature (for the NGC 5128 group from [ref] and [ref] ; the M81 group from [ref] ; for the M83 group from [ref] ; for the M106 group from [ref] , and for the Local Group from [ref] and [ref] ).
The extended halo of Centaurus A: uncovering satellites, streams, and substructures · Cumulative Luminosity Functions of Galaxy Groups · 0.96
Cites as background 1 paper
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Other studies have explored the NGC 5128 group [ref] , the M 106 group [ref] , the NGC 1023 group [ref] , and the M 101 group [ref] .
The extended halo of Centaurus A: uncovering satellites, streams, and substructures · Introduction · 0.96
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