New NIR light-curve templates for classical Cepheids

L. Inno, N. Matsunaga, M. Romaniello, G. Bono, A. Monson, I. Ferraro, G. Iannicola, E. Persson, R. Buonanno, W. Freedman, W. Gieren, M. A. T. Groenewegen, Y. Ita, C. D. Laney, B. Lemasle, B. F. Madore, T. Nagayama, Y. Nakada, M. Nonino, G. Pietrzyński & 5 others F. Primas, V. Scowcroft, I. Soszyński, T. Tanabé, A. Udalski

Research output: Contribution to journalArticle

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Abstract

Aims. We present new near-infrared (NIR) light-curve templates for fundamental (FU, J, H, KS) and first overtone (FO, J) classical Cepheids. The new templates together with period-luminosity and period-Wesenheit (PW) relations provide Cepheid distances from single-epoch observations with a precision only limited by the intrinsic accuracy of the method adopted.

Methods. The templates rely on a very large set of Galactic and Magellanic Cloud Cepheids (FU, ~600; FO, ~200) with well-sampled NIR (IRSF data set) and optical (V, I; OGLE data set) light-curves. To properly trace the change in the shape of the light-curve as a function of pulsation period, we split the sample of calibrating Cepheids into ten different period bins. The templates for the first time cover FO Cepheids and the short-period range of FU Cepheids (P ≤ 5 days). Moreover, the phase zero-point is anchored to the phase of the mean magnitude along the rising branch. The new approach has several advantages in sampling the light-curve of bump Cepheids when compared with the canonical phase of maximum light. We also provide new empirical estimates of the NIR-to-optical amplitude ratios for FU and FO Cepheids. We perform detailed analytical fits using seventh-order Fourier series and multi-Gaussian periodic functions. The latter are characterized by fewer free parameters (nine vs. fifteen).

Results. The mean NIR magnitudes based on the new templates are up to 80% more accurate than single-epoch NIR measurements and up to 50% more accurate than the mean magnitudes based on previous NIR templates, with typical associated uncertainties ranging from 0.015 mag (J band) to 0.019 mag (KS band). Moreover, we find that errors on individual distance estimates for Small Magellanic Cloud Cepheids derived from NIR PW relations are essentially reduced to the intrinsic scatter of the adopted relations.

Conclusions. Thus, the new templates are the ultimate tool for estimating precise Cepheid distances from NIR single-epoch observations, which can be safely adopted for future interesting applications, including deriving the 3D structure of the Magellanic Clouds.
Original languageEnglish
Article numberA30
JournalAstronomy & Astrophysics
Volume576
DOIs
Publication statusPublished - 1 Apr 2015

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light curve
near infrared
templates
Magellanic clouds
time measurement
periodic functions
Fourier series
calibrating
estimates
estimating
sampling
luminosity
harmonics

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Inno, L., Matsunaga, N., Romaniello, M., Bono, G., Monson, A., Ferraro, I., ... Udalski, A. (2015). New NIR light-curve templates for classical Cepheids. Astronomy & Astrophysics, 576, [A30]. https://doi.org/10.1051/0004-6361/201424396

New NIR light-curve templates for classical Cepheids. / Inno, L.; Matsunaga, N.; Romaniello, M.; Bono, G.; Monson, A.; Ferraro, I.; Iannicola, G.; Persson, E.; Buonanno, R.; Freedman, W.; Gieren, W.; Groenewegen, M. A. T.; Ita, Y.; Laney, C. D.; Lemasle, B.; Madore, B. F.; Nagayama, T.; Nakada, Y.; Nonino, M.; Pietrzyński, G.; Primas, F.; Scowcroft, V.; Soszyński, I.; Tanabé, T.; Udalski, A.

In: Astronomy & Astrophysics, Vol. 576, A30, 01.04.2015.

Research output: Contribution to journalArticle

Inno, L, Matsunaga, N, Romaniello, M, Bono, G, Monson, A, Ferraro, I, Iannicola, G, Persson, E, Buonanno, R, Freedman, W, Gieren, W, Groenewegen, MAT, Ita, Y, Laney, CD, Lemasle, B, Madore, BF, Nagayama, T, Nakada, Y, Nonino, M, Pietrzyński, G, Primas, F, Scowcroft, V, Soszyński, I, Tanabé, T & Udalski, A 2015, 'New NIR light-curve templates for classical Cepheids', Astronomy & Astrophysics, vol. 576, A30. https://doi.org/10.1051/0004-6361/201424396
Inno L, Matsunaga N, Romaniello M, Bono G, Monson A, Ferraro I et al. New NIR light-curve templates for classical Cepheids. Astronomy & Astrophysics. 2015 Apr 1;576. A30. https://doi.org/10.1051/0004-6361/201424396
Inno, L. ; Matsunaga, N. ; Romaniello, M. ; Bono, G. ; Monson, A. ; Ferraro, I. ; Iannicola, G. ; Persson, E. ; Buonanno, R. ; Freedman, W. ; Gieren, W. ; Groenewegen, M. A. T. ; Ita, Y. ; Laney, C. D. ; Lemasle, B. ; Madore, B. F. ; Nagayama, T. ; Nakada, Y. ; Nonino, M. ; Pietrzyński, G. ; Primas, F. ; Scowcroft, V. ; Soszyński, I. ; Tanabé, T. ; Udalski, A. / New NIR light-curve templates for classical Cepheids. In: Astronomy & Astrophysics. 2015 ; Vol. 576.
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abstract = "Aims. We present new near-infrared (NIR) light-curve templates for fundamental (FU, J, H, KS) and first overtone (FO, J) classical Cepheids. The new templates together with period-luminosity and period-Wesenheit (PW) relations provide Cepheid distances from single-epoch observations with a precision only limited by the intrinsic accuracy of the method adopted.Methods. The templates rely on a very large set of Galactic and Magellanic Cloud Cepheids (FU, ~600; FO, ~200) with well-sampled NIR (IRSF data set) and optical (V, I; OGLE data set) light-curves. To properly trace the change in the shape of the light-curve as a function of pulsation period, we split the sample of calibrating Cepheids into ten different period bins. The templates for the first time cover FO Cepheids and the short-period range of FU Cepheids (P ≤ 5 days). Moreover, the phase zero-point is anchored to the phase of the mean magnitude along the rising branch. The new approach has several advantages in sampling the light-curve of bump Cepheids when compared with the canonical phase of maximum light. We also provide new empirical estimates of the NIR-to-optical amplitude ratios for FU and FO Cepheids. We perform detailed analytical fits using seventh-order Fourier series and multi-Gaussian periodic functions. The latter are characterized by fewer free parameters (nine vs. fifteen).Results. The mean NIR magnitudes based on the new templates are up to 80{\%} more accurate than single-epoch NIR measurements and up to 50{\%} more accurate than the mean magnitudes based on previous NIR templates, with typical associated uncertainties ranging from 0.015 mag (J band) to 0.019 mag (KS band). Moreover, we find that errors on individual distance estimates for Small Magellanic Cloud Cepheids derived from NIR PW relations are essentially reduced to the intrinsic scatter of the adopted relations.Conclusions. Thus, the new templates are the ultimate tool for estimating precise Cepheid distances from NIR single-epoch observations, which can be safely adopted for future interesting applications, including deriving the 3D structure of the Magellanic Clouds.",
author = "L. Inno and N. Matsunaga and M. Romaniello and G. Bono and A. Monson and I. Ferraro and G. Iannicola and E. Persson and R. Buonanno and W. Freedman and W. Gieren and Groenewegen, {M. A. T.} and Y. Ita and Laney, {C. D.} and B. Lemasle and Madore, {B. F.} and T. Nagayama and Y. Nakada and M. Nonino and G. Pietrzyński and F. Primas and V. Scowcroft and I. Soszyński and T. Tanab{\'e} and A. Udalski",
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T1 - New NIR light-curve templates for classical Cepheids

AU - Inno, L.

AU - Matsunaga, N.

AU - Romaniello, M.

AU - Bono, G.

AU - Monson, A.

AU - Ferraro, I.

AU - Iannicola, G.

AU - Persson, E.

AU - Buonanno, R.

AU - Freedman, W.

AU - Gieren, W.

AU - Groenewegen, M. A. T.

AU - Ita, Y.

AU - Laney, C. D.

AU - Lemasle, B.

AU - Madore, B. F.

AU - Nagayama, T.

AU - Nakada, Y.

AU - Nonino, M.

AU - Pietrzyński, G.

AU - Primas, F.

AU - Scowcroft, V.

AU - Soszyński, I.

AU - Tanabé, T.

AU - Udalski, A.

PY - 2015/4/1

Y1 - 2015/4/1

N2 - Aims. We present new near-infrared (NIR) light-curve templates for fundamental (FU, J, H, KS) and first overtone (FO, J) classical Cepheids. The new templates together with period-luminosity and period-Wesenheit (PW) relations provide Cepheid distances from single-epoch observations with a precision only limited by the intrinsic accuracy of the method adopted.Methods. The templates rely on a very large set of Galactic and Magellanic Cloud Cepheids (FU, ~600; FO, ~200) with well-sampled NIR (IRSF data set) and optical (V, I; OGLE data set) light-curves. To properly trace the change in the shape of the light-curve as a function of pulsation period, we split the sample of calibrating Cepheids into ten different period bins. The templates for the first time cover FO Cepheids and the short-period range of FU Cepheids (P ≤ 5 days). Moreover, the phase zero-point is anchored to the phase of the mean magnitude along the rising branch. The new approach has several advantages in sampling the light-curve of bump Cepheids when compared with the canonical phase of maximum light. We also provide new empirical estimates of the NIR-to-optical amplitude ratios for FU and FO Cepheids. We perform detailed analytical fits using seventh-order Fourier series and multi-Gaussian periodic functions. The latter are characterized by fewer free parameters (nine vs. fifteen).Results. The mean NIR magnitudes based on the new templates are up to 80% more accurate than single-epoch NIR measurements and up to 50% more accurate than the mean magnitudes based on previous NIR templates, with typical associated uncertainties ranging from 0.015 mag (J band) to 0.019 mag (KS band). Moreover, we find that errors on individual distance estimates for Small Magellanic Cloud Cepheids derived from NIR PW relations are essentially reduced to the intrinsic scatter of the adopted relations.Conclusions. Thus, the new templates are the ultimate tool for estimating precise Cepheid distances from NIR single-epoch observations, which can be safely adopted for future interesting applications, including deriving the 3D structure of the Magellanic Clouds.

AB - Aims. We present new near-infrared (NIR) light-curve templates for fundamental (FU, J, H, KS) and first overtone (FO, J) classical Cepheids. The new templates together with period-luminosity and period-Wesenheit (PW) relations provide Cepheid distances from single-epoch observations with a precision only limited by the intrinsic accuracy of the method adopted.Methods. The templates rely on a very large set of Galactic and Magellanic Cloud Cepheids (FU, ~600; FO, ~200) with well-sampled NIR (IRSF data set) and optical (V, I; OGLE data set) light-curves. To properly trace the change in the shape of the light-curve as a function of pulsation period, we split the sample of calibrating Cepheids into ten different period bins. The templates for the first time cover FO Cepheids and the short-period range of FU Cepheids (P ≤ 5 days). Moreover, the phase zero-point is anchored to the phase of the mean magnitude along the rising branch. The new approach has several advantages in sampling the light-curve of bump Cepheids when compared with the canonical phase of maximum light. We also provide new empirical estimates of the NIR-to-optical amplitude ratios for FU and FO Cepheids. We perform detailed analytical fits using seventh-order Fourier series and multi-Gaussian periodic functions. The latter are characterized by fewer free parameters (nine vs. fifteen).Results. The mean NIR magnitudes based on the new templates are up to 80% more accurate than single-epoch NIR measurements and up to 50% more accurate than the mean magnitudes based on previous NIR templates, with typical associated uncertainties ranging from 0.015 mag (J band) to 0.019 mag (KS band). Moreover, we find that errors on individual distance estimates for Small Magellanic Cloud Cepheids derived from NIR PW relations are essentially reduced to the intrinsic scatter of the adopted relations.Conclusions. Thus, the new templates are the ultimate tool for estimating precise Cepheid distances from NIR single-epoch observations, which can be safely adopted for future interesting applications, including deriving the 3D structure of the Magellanic Clouds.

UR - http://dx.doi.org/10.1051/0004-6361/201424396

UR - http://dx.doi.org/10.1051/0004-6361/201424396

U2 - 10.1051/0004-6361/201424396

DO - 10.1051/0004-6361/201424396

M3 - Article

VL - 576

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

M1 - A30

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