China-Chile Proposal - 版本历史

2019年6月26日 (三) 00:43 Shen

2019-06-26T00:43:27Z

←上一版本		2019年6月26日 (三) 00:43的版本
第1行：		第1行：
	'''China-Chile Joint Research Fund 2016'''		'''China-Chile Joint Research Fund 2016'''

	'''[[2019 ~~ChePanmodel~~ workshop]]'''		'''[[2019 ChePanModel workshop]]'''

	=Exploring the Star Formation Histories of Galaxies in Different Environments from MaNGA Spectra=		=Exploring the Star Formation Histories of Galaxies in Different Environments from MaNGA Spectra=

2019年6月26日 (三) 00:43 Shen

2019-06-26T00:43:03Z

←上一版本		2019年6月26日 (三) 00:43的版本
第1行：		第1行：
	'''China-Chile Joint Research Fund 2016'''		'''China-Chile Joint Research Fund 2016'''

			'''[[2019 ChePanmodel workshop]]'''

	=Exploring the Star Formation Histories of Galaxies in Different Environments from MaNGA Spectra=		=Exploring the Star Formation Histories of Galaxies in Different Environments from MaNGA Spectra=

Cluster：/* Implementation Plan of research */

2016-11-01T05:20:46Z

Implementation Plan of research

←上一版本		2016年11月1日 (二) 05:20的版本
第129行：		第129行：
	1. 2017.1-2017.9, construction of the sample and reducing MaNGA data. Galaxies that have already been observed by MaNGA will be collected. Radial binning or other binning method will be applied to MaNGA datacube. UV to IR data will be collected from GALEX, Spitzer, WISE and other observations. At the same time, we will develop CIGALE code, making it to be able to fit both spectrocsopic and photometric data. The spectral and SED of isolated and paired galaxies will be fitted. Parameters such as the star formation history, dust extinction, rotation velocity and velocity dispersion will be discussed.		1. 2017.1-2017.9, construction of the sample and reducing MaNGA data. Galaxies that have already been observed by MaNGA will be collected. Radial binning or other binning method will be applied to MaNGA datacube. UV to IR data will be collected from GALEX, Spitzer, WISE and other observations. At the same time, we will develop CIGALE code, making it to be able to fit both spectrocsopic and photometric data. The spectral and SED of isolated and paired galaxies will be fitted. Parameters such as the star formation history, dust extinction, rotation velocity and velocity dispersion will be discussed.

	2. 2017.10-2017.12, publish the first paper, presenting the fitting results. Comparing the difference between isolated and paired galaxies. Discussing the spatial distribution of the parameters obtained from fitting. Discussing the uncertainties of the fitting.		2. 2017.10-2017.12, publish the first paper, presenting the fitting results. Comparing the difference between isolated and paired galaxies. Discussing the spatial distribution of the parameters obtained from fitting. Discussing the uncertainties of the fitting. Celebrating a workshop in Chile.

	3. 2018.1-2018.9, introducing chemical evolution to the fitting method.		3. 2018.1-2018.9, introducing chemical evolution to the fitting method. Comparing the results with/without the consideration of chemical evolution. The environmental dependence of physical properties will be studied.

			4. 2018.10-2018.12, publish the second paper. Summary of the work. Celebrating a workshop in China.
	4. 2018.10-2018.12

			Both University of Antofagasta and Shanghai Astronomical Observatory have fast network and an enough amount of computing power for conducting the project.

	== Itemized budget ==		== Itemized budget ==

Cluster：/* Implementation Plan of research */

2016-11-01T03:27:01Z

Implementation Plan of research

←上一版本		2016年11月1日 (二) 03:27的版本
第126行：		第126行：

	We divide this project into 4 phases, listed below:		We divide this project into 4 phases, listed below:
	1. 2017.1-2017.7

			1. 2017.1-2017.9, construction of the sample and reducing MaNGA data. Galaxies that have already been observed by MaNGA will be collected. Radial binning or other binning method will be applied to MaNGA datacube. UV to IR data will be collected from GALEX, Spitzer, WISE and other observations. At the same time, we will develop CIGALE code, making it to be able to fit both spectrocsopic and photometric data. The spectral and SED of isolated and paired galaxies will be fitted. Parameters such as the star formation history, dust extinction, rotation velocity and velocity dispersion will be discussed.
	2. 2017.8-2017.12

			2. 2017.10-2017.12, publish the first paper, presenting the fitting results. Comparing the difference between isolated and paired galaxies. Discussing the spatial distribution of the parameters obtained from fitting. Discussing the uncertainties of the fitting.
⚫	3. 2018.1-2018.7

			3. 2018.1-2018.9, introducing chemical evolution to the fitting method.
	4. 2018.8-2018.12

		⚫	4. 2018.10-2018.12

	== Itemized budget ==		== Itemized budget ==

Cluster：/* Implementation Plan of research */

2016-11-01T03:10:28Z

Implementation Plan of research

←上一版本		2016年11月1日 (二) 03:10的版本
第124行：		第124行：

	Part of the budget will be also used to cover the expenses generated by observing runs (travels, masks, etc) for possible follow-up observations of our galaxy targets.		Part of the budget will be also used to cover the expenses generated by observing runs (travels, masks, etc) for possible follow-up observations of our galaxy targets.

			We divide this project into 4 phases, listed below:
			1. 2017.1-2017.7

			2. 2017.8-2017.12

			3. 2018.1-2018.7

			4. 2018.8-2018.12

	== Itemized budget ==		== Itemized budget ==

Cluster：/* List of publications */

2016-10-31T08:30:33Z

List of publications

←上一版本		2016年10月31日 (一) 08:30的版本
第154行：		第154行：
	#‘’Catalogues of isolated galaxies, isolated pairs, and isolated triplets in the local Universe’’ , M. Argudo-Fernández; S. Verley; G. Bergond; S. Duarte Puertas; E. Ramos Carmona; J. Sabater; M. Fernández Lorenzo; D. Espada; J. Sulentic; J. E. Ruiz; S. Leon, A&A, 578A, 110A (2015)		#‘’Catalogues of isolated galaxies, isolated pairs, and isolated triplets in the local Universe’’ , M. Argudo-Fernández; S. Verley; G. Bergond; S. Duarte Puertas; E. Ramos Carmona; J. Sabater; M. Fernández Lorenzo; D. Espada; J. Sulentic; J. E. Ruiz; S. Leon, A&A, 578A, 110A (2015)
	#‘’Isolated Galaxies versus Interacting Pairs with MaNGA’’ , M. Argudo- Fernández, F. Yuan, S. Shen, J. Yin, R. Chang, S. Feng, Galaxies, 3, 156F (2015).		#‘’Isolated Galaxies versus Interacting Pairs with MaNGA’’ , M. Argudo- Fernández, F. Yuan, S. Shen, J. Yin, R. Chang, S. Feng, Galaxies, 3, 156F (2015).
	#‘’A sample of galaxy pairs ~~identi ed~~ from the LAMOST spectral survey and the Sloan Digital Sky Survey’’ , Shiyin Shen, M. Argudo-Fernandez, Li Chen et al., RAA, 16c, 7S (2016).		#‘’A sample of galaxy pairs identified from the LAMOST spectral survey and the Sloan Digital Sky Survey’’ , Shiyin Shen, M. Argudo-Fernandez, Li Chen et al., RAA, 16c, 7S (2016).
	#‘’An Isolated Compact Galaxy Triplet’’, Shuai Feng, Zheng-Yi Shao, Shi-Yin Shen, Maria Argudo-Fernandez, Hong Wu, Man-I Lam, Ming Yang, and Fang-Ting Yuan, RAA, 16e, 3F (2016).		#‘’An Isolated Compact Galaxy Triplet’’, Shuai Feng, Zheng-Yi Shao, Shi-Yin Shen, Maria Argudo-Fernandez, Hong Wu, Man-I Lam, Ming Yang, and Fang-Ting Yuan, RAA, 16e, 3F (2016).
	#‘’Effects of local and large-scale environments on nuclear activity and star formation’’ , M. Argudo-Fernández; S. Shen; J. Sabater; S. Duarte Puertas; S. Verley, A&A, 592A, 30A (2016).		#‘’Effects of local and large-scale environments on nuclear activity and star formation’’ , M. Argudo-Fernández; S. Shen; J. Sabater; S. Duarte Puertas; S. Verley, A&A, 592A, 30A (2016).
	#‘’SDSS-IV MaNGA: Properties of galaxies with kinematically decoupled stellar and gaseous components’’, Jin, Yifei; Chen, Yanmei; Shi, Yong; et al., MNRAS, accepted (2016).		#‘’SDSS-IV MaNGA: Properties of galaxies with kinematically decoupled stellar and gaseous components’’, Jin, Yifei; Chen, Yanmei; Shi, Yong; et al., MNRAS, accepted (2016).
	#‘’The growth of the central region by acquisition of counter-rotating gas ~~innstar~~-forming galaxies,’’ YanMei Chen; Yong Shi; C. A. Tremonti et al., submitted to Nature.		#‘’The growth of the central region by acquisition of counter-rotating gas in star-forming galaxies,’’ YanMei Chen; Yong Shi; C. A. Tremonti et al., submitted to Nature.
	#‘’Stellar Population Gradients as a Function of Galaxy Mass and Environment’’, D, Goddard; D. Thomas, C. Maraston et al., submitted to MNRAS.		#‘’Stellar Population Gradients as a Function of Galaxy Mass and Environment’’, D, Goddard; D. Thomas, C. Maraston et al., submitted to MNRAS.
	#‘’Spatially Resolved Star Formation Histories in Galaxies as a Function of Galaxy Mass and Type’’, D, Goddard; D. Thomas, C. Maraston et al., submitted to MNRAS.		#‘’Spatially Resolved Star Formation Histories in Galaxies as a Function of Galaxy Mass and Type’’, D, Goddard; D. Thomas, C. Maraston et al., submitted to MNRAS.
	#‘’Star Formation History of the Galaxy Merger Mrk848 with SDSS-IV MaNGA’’, F. Yuan; S. Shen; L. Hao; Maria Argudo-Fernandez, in preparation.		#‘’Star Formation History of the Galaxy Merger Mrk848 with SDSS-IV MaNGA’’, F.-T. Yuan; S. Shen; L. Hao; Maria Argudo-Fernandez, in preparation.
	#‘’Star formation histories of isolated galaxies with MaNGA’’, Maria Argudo-Fernandez; M. Boquien; S. Shen; F. Yuan, J. Yin, R. Chang, K. Bundy, C. Liu, in preparation.		#‘’Star formation histories of isolated galaxies with MaNGA’’, Maria Argudo-Fernandez; M. Boquien; S. Shen; F.-T. Yuan, J. Yin, R. Chang, K. Bundy, C. Liu, in preparation.

	[[Category:Internal]]		[[Category:Internal]]

Cluster：/* Environmental effects on star formation properties in galaxy pairs */

2016-10-31T08:23:43Z

Environmental effects on star formation properties in galaxy pairs

←上一版本		2016年10月31日 (一) 08:23的版本
第109行：		第109行：
	Merging is a presumably cause to transfer blue and star-forming galaxies to red and dead galaxies. Simulations show that the interaction of two galaxies in a pair can cause the gas inflow, triggering starbursts in the central regions of galaxies. While numerous observations have found that there is enhancement of star formation in galaxy pairs, the enhancement may depend on the local environment (see e.g. Tonneson et al., 2014). Also, the spatial extent of the enhanced star formation in pairs is still not clear. Although many studies found enhanced star formation in central regions, there are also cases showing star formation widely spread to bridge and tidal tail regions (e.g. Boquien et al. 2007, 2009, 2010, Smith et al. 2010, 2016). A recent work by Moreno et al. (2015) shows that pair interactions can cause the enhancement of star formation in the center, but at the same time suppress the activity at outskirts.		Merging is a presumably cause to transfer blue and star-forming galaxies to red and dead galaxies. Simulations show that the interaction of two galaxies in a pair can cause the gas inflow, triggering starbursts in the central regions of galaxies. While numerous observations have found that there is enhancement of star formation in galaxy pairs, the enhancement may depend on the local environment (see e.g. Tonneson et al., 2014). Also, the spatial extent of the enhanced star formation in pairs is still not clear. Although many studies found enhanced star formation in central regions, there are also cases showing star formation widely spread to bridge and tidal tail regions (e.g. Boquien et al. 2007, 2009, 2010, Smith et al. 2010, 2016). A recent work by Moreno et al. (2015) shows that pair interactions can cause the enhancement of star formation in the center, but at the same time suppress the activity at outskirts.

	We select the pair sample from the catalog of groups constructed by Yang et al. (2007) based on SDSS-DR7 data. The spectroscopic redshifts for the companion galaxies are collected not only from SDSS-DR7, but also SDSS-DR10, NED, and LAMOST, in order to minimize the fiber collision effect which causes the missing of the spectrum of one member galaxy in a close pair. Especially, the LAMOST data are obtained through the project dedicated to complement the spectroscopic redshifts of SDSS close pairs with LAMOST spectroscopy (Shen et al. 2016). Two galaxies are selected as a pair if they satisfy the following criteria: 1) Both galaxies have spectroscopic redshifts; 2) The projected separation rp is less than 50 kpc; 3) The velocity difference dv is less than 500 km/s. A part of this sample (including approximately 1000 galaxies) is selected for MaNGA observations over the course of the survey.		We select the pair sample from the catalog of groups constructed by Yang et al. (2007) based on SDSS-DR7 data. The spectroscopic redshifts for the companion galaxies are collected not only from SDSS-DR7, but also SDSS-DR10, NED, and LAMOST, in order to minimize the fiber collision effect which causes the missing of the spectrum of one member galaxy in a close pair. Especially, the LAMOST data are obtained through the project dedicated to complement the spectroscopic redshifts of SDSS close pairs with LAMOST spectroscopy (Shen et al. 2016). Two galaxies are selected as a pair if they satisfy the following criteria: 1) Both galaxies have spectroscopic redshifts; 2) The projected separation (r_p) is less than 50 kpc; 3) The velocity difference (dV) is less than 500 km/s. A part of this sample (including approximately 1000 galaxies) is selected for MaNGA observations over the course of the survey.

	We focus on exploring how the environment affects the properties in galaxy close pairs. Yang et al. (2007)’s group catalog already provides us with halo mass of each pairs, which can be used as a parameter to indicate the environment. We also use tidal strength parameters that measure the local galaxy density of each pair (Argudo-Fernández et al., 2015) as another approach to describe the environment. Based on this SDSS pair sample, we can statistically explore the environmental dependence of pairs. On the other hand, MaNGA IFU allows us to study the spatially resolved properties of galaxies, and therefore can further help us clarify in which part the SFR/dust is changed, and whether the spatial variation has some dependence on the environment.		We focus on exploring how the environment affects the properties in galaxy close pairs. Yang et al. (2007)'s group catalog already provides us with halo mass of each pairs, which can be used as a parameter to indicate the environment. We also use tidal strength parameters that measure the local galaxy density of each pair (Argudo-Fernández et al., 2015) as another approach to describe the environment. Based on this SDSS pair sample, we can statistically explore the environmental dependence of pairs. On the other hand, MaNGA IFU allows us to study the spatially resolved properties of galaxies, and therefore can further help us clarify in which part the SFR/dust is changed, and whether the spatial variation has some dependence on the environment.

	== Implementation Plan of research ==		== Implementation Plan of research ==

Cluster：/* Spectro-photometric modeling */

2016-10-31T07:18:20Z

Spectro-photometric modeling

←上一版本		2016年10月31日 (一) 07:18的版本
第71行：		第71行：
	We have to note that our team is no stranger to the combination of spectral and photometric data. Doing so in a groundwork for this proposal, we have studied the SFH of a galaxy merger observed with MaNGA. Galaxy mergers play an important role in the formation and evolution of galaxies and their dark matter halos. The UV and IR data are used to constrain the star formation rate and dust attenuation for mergers, which are tracers of the evolutionary stage of the systems. However, spatially resolved studies of galaxy mergers are restricted to very close galaxies, especially due to the lack spatial resolution in IR data. In Yuan et al. (in preparation), we show how the use of UV-to-IR broadband SED (see Figure 3), in combination with MaNGA IFS (see Figure 4), provide unique opportunity to study the star formation histories and dust attenuation at the tail and core parts of the merging galaxy Mrk 848.		We have to note that our team is no stranger to the combination of spectral and photometric data. Doing so in a groundwork for this proposal, we have studied the SFH of a galaxy merger observed with MaNGA. Galaxy mergers play an important role in the formation and evolution of galaxies and their dark matter halos. The UV and IR data are used to constrain the star formation rate and dust attenuation for mergers, which are tracers of the evolutionary stage of the systems. However, spatially resolved studies of galaxy mergers are restricted to very close galaxies, especially due to the lack spatial resolution in IR data. In Yuan et al. (in preparation), we show how the use of UV-to-IR broadband SED (see Figure 3), in combination with MaNGA IFS (see Figure 4), provide unique opportunity to study the star formation histories and dust attenuation at the tail and core parts of the merging galaxy Mrk 848.

	[[File:~~Mrk848Photo~~.~~png~~]]		[[File:Mrk848Photo2.PNG]]

	Figure 3: Fitting results by CIGALE for the regions 1, 2, and 3 of the merger Mrk 848 from GALEX, ugriz SDSS bands, and IRAC data. Black dots are observed band fluxes. Red lines indicate the results of SED fitting assuming a two exponentially decreasing SFH. Yellow lines indicate the results of SED fitting assuming a delayed SFH.		Figure 3: Fitting results by CIGALE for the regions 1, 2, and 3 of the merger Mrk 848 from GALEX, ugriz SDSS bands, and IRAC data. Black dots are observed band fluxes. Red lines indicate the results of SED fitting assuming a two exponentially decreasing SFH. Yellow lines indicate the results of SED fitting assuming a delayed SFH.

Cluster：/* Spectro-photometric modeling */

2016-10-31T06:53:27Z

Spectro-photometric modeling

←上一版本		2016年10月31日 (一) 06:53的版本
第67行：		第67行：
	To enjoy the synergistic benefits of both approaches, we will develop a new version of CIGALE that will be able to simultaneously fit both broadband and spectra. By combining optical spectra with UV-to-IR broadband observations, this new resource will allow us to get a better handle on the continuum attenuation, since the Balmer decrement is only for the ionised gas and the conversion to a continuum attenuation is uncertain, and break more reliably the age-attenuation degeneracy, among other things. Therefore, used in combination with spatially resolved multi-wavelength data to complement MaNGA observations, this will allow us to obtain better estimates on the SFR, the SFH, and other physical properties of nearby galaxies. As with current versions of CIGALE, this code will be made freely available.		To enjoy the synergistic benefits of both approaches, we will develop a new version of CIGALE that will be able to simultaneously fit both broadband and spectra. By combining optical spectra with UV-to-IR broadband observations, this new resource will allow us to get a better handle on the continuum attenuation, since the Balmer decrement is only for the ionised gas and the conversion to a continuum attenuation is uncertain, and break more reliably the age-attenuation degeneracy, among other things. Therefore, used in combination with spatially resolved multi-wavelength data to complement MaNGA observations, this will allow us to obtain better estimates on the SFR, the SFH, and other physical properties of nearby galaxies. As with current versions of CIGALE, this code will be made freely available.

	~~One~~ the modification carried out, we will model the MaNGA galaxies present in our subsample (see in particular Sect. 2.2 and 2.3) and measure their spatially resolved physical properties (SFR over different timescales, metallicities [see also Sect. 2.2.2], dust attenuation, stellar masses, etc.). This will serve as a basis for the investigation of the effect of the environment on the evolution of galaxies.		Once the modification carried out, we will model the MaNGA galaxies present in our subsample (see in particular Sect. 2.2 and 2.3) and measure their spatially resolved physical properties (SFR over different timescales, metallicities [see also Sect. 2.2.2], dust attenuation, stellar masses, etc.). This will serve as a basis for the investigation of the effect of the environment on the evolution of galaxies.

	We have to note that our team is no stranger to the combination of spectral and photometric data. Doing so in a groundwork for this proposal, we have studied the SFH of a galaxy merger observed with MaNGA. Galaxy mergers play an important role in the formation and evolution of galaxies and their dark matter halos. The UV and IR data are used to constrain the star formation rate and dust attenuation for mergers, which are tracers of the evolutionary stage of the systems. However, spatially resolved studies of galaxy mergers are restricted to very close galaxies, especially due to the lack spatial resolution in IR data. In Yuan et al. (in preparation), we show how the use of UV-to-IR broadband SED (see Figure 3), in combination with MaNGA IFS (see Figure 4), provide unique opportunity to study the star formation histories and dust attenuation at the tail and core parts of the merging galaxy Mrk 848.		We have to note that our team is no stranger to the combination of spectral and photometric data. Doing so in a groundwork for this proposal, we have studied the SFH of a galaxy merger observed with MaNGA. Galaxy mergers play an important role in the formation and evolution of galaxies and their dark matter halos. The UV and IR data are used to constrain the star formation rate and dust attenuation for mergers, which are tracers of the evolutionary stage of the systems. However, spatially resolved studies of galaxy mergers are restricted to very close galaxies, especially due to the lack spatial resolution in IR data. In Yuan et al. (in preparation), we show how the use of UV-to-IR broadband SED (see Figure 3), in combination with MaNGA IFS (see Figure 4), provide unique opportunity to study the star formation histories and dust attenuation at the tail and core parts of the merging galaxy Mrk 848.

Cluster：/* Abstract */

2016-10-24T18:27:26Z

Abstract

←上一版本		2016年10月24日 (一) 18:27的版本
第17行：		第17行：
	*Team		*Team

	Médéric Boquien(1) (PI), ~~Shiyin Shen~~(2) (PI), Maria Argudo-Fernández(1) (Co-I), ~~Fangting~~ ~~Yuan~~(2) (Co-I), Jun Yin(2) (Co-I), Ruixiang Chang(2) (Co-I), Lei Hao(2) (Co-I)		Médéric Boquien(1) (PI), Fangting Yuan(2) (PI), Maria Argudo-Fernández(1) (Co-I), Shiyin Shen(2) (Co-I), Jun Yin(2) (Co-I), Ruixiang Chang(2) (Co-I), Lei Hao(2) (Co-I)

	- University of Antofagasta, Chile		- University of Antofagasta, Chile

China-Chile Proposal - 版本历史

2019年6月26日 (三) 00:43 Shen

2019年6月26日 (三) 00:43 Shen

Cluster：​/* Implementation Plan of research */

Cluster：​/* Implementation Plan of research */

Cluster：​/* Implementation Plan of research */

Cluster：​/* List of publications */

Cluster：​/* Environmental effects on star formation properties in galaxy pairs */

Cluster：​/* Spectro-photometric modeling */

Cluster：​/* Spectro-photometric modeling */

Cluster：​/* Abstract */

Cluster：/* Implementation Plan of research */

Cluster：/* Implementation Plan of research */

Cluster：/* Implementation Plan of research */

Cluster：/* List of publications */

Cluster：/* Environmental effects on star formation properties in galaxy pairs */

Cluster：/* Spectro-photometric modeling */

Cluster：/* Spectro-photometric modeling */

Cluster：/* Abstract */