tests:streams:challenges
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| tests:streams:challenges [2015/08/29 18:33] – cmateu_astrosen.unam.mx | tests:streams:challenges [2022/10/24 12:26] (current) – external edit 127.0.0.1 | ||
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| * *.obs.* are convolved observable coordinates and error bars. The 11 columns are: apparent V magnitude, RA, dec, parallax, parallax error, proper motion in RA, PM_{RA} error, PM in dec, PM_{dec} error, RV, RV error. | * *.obs.* are convolved observable coordinates and error bars. The 11 columns are: apparent V magnitude, RA, dec, parallax, parallax error, proper motion in RA, PM_{RA} error, PM in dec, PM_{dec} error, RV, RV error. | ||
| * [[http:// | * [[http:// | ||
| - | * [[http:// | + | * [[http:// |
| * [[http:// | * [[http:// | ||
| * [[http:// | * [[http:// | ||
| Line 159: | Line 159: | ||
| * $M_{Halo} = 1.81194\times 10^{12}\, | * $M_{Halo} = 1.81194\times 10^{12}\, | ||
| - | * $R_{Halo} = 32260\,pc$ | + | * $r_{Halo} = 32260\,pc$ |
| * $q_z = 0.8140$ | * $q_z = 0.8140$ | ||
| * $M_{Pal5}(t=-4 Gyr) = 31090\, | * $M_{Pal5}(t=-4 Gyr) = 31090\, | ||
| * $M_{Pal5}(t=today) = 13150\, | * $M_{Pal5}(t=today) = 13150\, | ||
| * $d_{Sun} = 23190\,pc$ | * $d_{Sun} = 23190\,pc$ | ||
| - | * $V_C(R_{Sun}) = 249.01\, | + | * $V_C(r_{Sun}) = 249.01\, |
| - | * $V_C(R_{Pal5}) = 247.84\, | + | * $V_C(r_{Pal5}) = 247.84\, |
| - | * $V_C(R_{Halo}) = 251.99\, | + | * $V_C(r_{Halo}) = 251.99\, |
| - | * $a(R_{Sun}, 0, 0) = 7.95\, | + | * $a(r_{Sun}, 0, 0) = 7.95\, |
| - | * $a(R_{Pal5}) = a(7816 pc, 240 pc, 16640 pc) = 3.51\, | + | * $a(r_{Pal5}) = a(7816 pc, 240 pc, 16640 pc) = 3.51\, |
| - | * $a(R_{Halo}, 0, 0) = 2.06\, | + | * $a(r_{Halo}, 0, 0) = 2.06\, |
| | | ||
| == Functional form of the potential components == | == Functional form of the potential components == | ||
| Line 175: | Line 175: | ||
| Flattened NFW halo: | Flattened NFW halo: | ||
| - | * $\Phi_{Halo}(R, | + | * $\Phi_{Halo}(R, |
| Jaffe bulge: | Jaffe bulge: | ||
| - | * $\Phi_{Bulge} = \frac{GM_{Bulge}}{b_{bulge}}\ln{\frac{R}{R+b_{bulge}}$ | + | * $\Phi_{Bulge}(r) = \frac{GM_{Bulge}}{b_{bulge}}\ln{\frac{r}{r+b_{bulge}}$ |
| * $M_{Bulge} = 3.4\times 10^{10}\, | * $M_{Bulge} = 3.4\times 10^{10}\, | ||
| * $b_{Bulge} = 700.0\,pc$ | * $b_{Bulge} = 700.0\,pc$ | ||
| Line 185: | Line 185: | ||
| Miyamoto-Nagai disk: | Miyamoto-Nagai disk: | ||
| - | * $\Phi_{Disk} = -\frac{GM_{Disk}}{\sqrt{R^2+\left(a_{Disk}+\sqrt{z^2+b_{Disk}^2}\right)^2}}$ | + | * $\Phi_{Disk}(r) = -\frac{GM_{Disk}}{\sqrt{R^2+\left(a_{Disk}+\sqrt{z^2+b_{Disk}^2}\right)^2}}$ |
| * $M_{Disk} = 1.0\times 10^{11}\, | * $M_{Disk} = 1.0\times 10^{11}\, | ||
| * $a_{Disk} = 6500\,pc$ | * $a_{Disk} = 6500\,pc$ | ||
| Line 236: | Line 236: | ||
| Streams have been populated with one red KIII giant per 40 solar masses (Helmi et al. 2011; Marigo et al. 2008), with M_V = 1, V-I = 1. The sample includes stars with G band > 20, which would be outside of the Gaia limits. Removing these stars eliminates several of the streams. | Streams have been populated with one red KIII giant per 40 solar masses (Helmi et al. 2011; Marigo et al. 2008), with M_V = 1, V-I = 1. The sample includes stars with G band > 20, which would be outside of the Gaia limits. Removing these stars eliminates several of the streams. | ||
| - | ===halo star catalogue=== | + | ===Halo star catalogue=== |
| This is the whole stellar halo catalogue based on the Aquarius A-2 simulation. Details about how the catalogue is constructed can be found in Cooper et al. (2010). The catalogue includes all the accreted particles in the stellar halo. It is the parent catalogue used to make the 10 streams in the stream catalogue above. Again the Sun has been placed at 8 kpc with a velocity of (0, | This is the whole stellar halo catalogue based on the Aquarius A-2 simulation. Details about how the catalogue is constructed can be found in Cooper et al. (2010). The catalogue includes all the accreted particles in the stellar halo. It is the parent catalogue used to make the 10 streams in the stream catalogue above. Again the Sun has been placed at 8 kpc with a velocity of (0, | ||
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| - | ===complete | + | ===Complete |
| Each particle in the halo star catalogue above represents a stellar population instead of individual stars. We have further sampled these particles into individual stars and details about the sampling can be found in | Each particle in the halo star catalogue above represents a stellar population instead of individual stars. We have further sampled these particles into individual stars and details about the sampling can be found in | ||
| Line 258: | Line 258: | ||
| extracted from the Lowing et al. 2015 mock catalogues explained in the previous subsection. | extracted from the Lowing et al. 2015 mock catalogues explained in the previous subsection. | ||
| - | //Error prescriptions:// | + | //Error prescriptions:// |
| The SQL queries used to extract the stars are provided as part of each file’s header. | The SQL queries used to extract the stars are provided as part of each file’s header. | ||
| Line 347: | Line 347: | ||
| Here are two mock catalogues for K giant stars in two Haloes from Andreea Font's LJMU Gas-Dynamical simulations (Font et al. in prep). We have used the same methods as for the [[# | Here are two mock catalogues for K giant stars in two Haloes from Andreea Font's LJMU Gas-Dynamical simulations (Font et al. in prep). We have used the same methods as for the [[# | ||
| - | //Error prescriptions:// | + | //Error prescriptions:// |
| The SQL queries used to extract the stars are provided as part of each file’s header. | The SQL queries used to extract the stars are provided as part of each file’s header. | ||
tests/streams/challenges.1440873236.txt.gz · Last modified: 2022/10/24 12:26 (external edit)