Table 5
Open in new tab

Location and 3D motion of IRAS 18286|$-$|0959 in the Milky Way estimated from the VERA astrometry.

ParameterValue
Galactic coordinates, (⁠|$ l$| , |$ b$| ) [|$ ^{\circ}$| ]*(21.80, |$-$| 0.13)
Heliocentric distance, |$ D$| [kpc]*3.61 |$ \pm$| 0.63
Systemic LSR velocity, |$ V_{\rm sys}$| [km s|$ ^{-1}$| ]*60 |$ \pm$| 5
|$ R_{\rm0}$| [kpc]†8.0
|$ \Theta_{\rm0}$| [km s|$ ^{-1}$| ]†220
(⁠|$ U_{\odot}$| , |$ V_{\odot}$| , |$ W_{\odot}$| ) [km s|$ ^{-1}$| ]‡(7.5, 13.5, 6.8)
|$ z_{\rm0}$| [pc]§16
|$ R_{\rm gal}$| [kpc]4.84 |$ \pm$| 0.50
|$ z$| [pc]7 |$ \pm$| 1
Case 1: fixed in the system
|$ V_{R}$| [km s|$ ^{-1}$| ]66 |$ \pm$| 19
|$ V_{\theta}$| [km s|$ ^{-1}$| ]148 |$ \pm$| 25
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 1 |$ \pm$| 20
Case 2: moving in (⁠|$-$| 0.76, |$-$| 1.23) [mas yr|$ ^{-1}$| ] with respect
to the system (result of the kinematical model fitting)
|$ V_{R}$| [km s|$ ^{-1}$| ]51 |$ \pm$| 17
|$ V_{\theta}$| [km s|$ ^{-1}$| ]169 |$ \pm$| 22
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 2 |$ \pm$| 20
Case 3: moving in (⁠|$-$| 3, |$-$| 5) [mas yr|$ ^{-1}$| ]
with respect to the system
|$ V_{R}$| [km s|$ ^{-1}$| ]6 |$ \pm$| 13
|$ V_{\theta}$| [km s|$ ^{-1}$| ]228 |$ \pm$| 17
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 7 |$ \pm$| 20
ParameterValue
Galactic coordinates, (⁠|$ l$| , |$ b$| ) [|$ ^{\circ}$| ]*(21.80, |$-$| 0.13)
Heliocentric distance, |$ D$| [kpc]*3.61 |$ \pm$| 0.63
Systemic LSR velocity, |$ V_{\rm sys}$| [km s|$ ^{-1}$| ]*60 |$ \pm$| 5
|$ R_{\rm0}$| [kpc]†8.0
|$ \Theta_{\rm0}$| [km s|$ ^{-1}$| ]†220
(⁠|$ U_{\odot}$| , |$ V_{\odot}$| , |$ W_{\odot}$| ) [km s|$ ^{-1}$| ]‡(7.5, 13.5, 6.8)
|$ z_{\rm0}$| [pc]§16
|$ R_{\rm gal}$| [kpc]4.84 |$ \pm$| 0.50
|$ z$| [pc]7 |$ \pm$| 1
Case 1: fixed in the system
|$ V_{R}$| [km s|$ ^{-1}$| ]66 |$ \pm$| 19
|$ V_{\theta}$| [km s|$ ^{-1}$| ]148 |$ \pm$| 25
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 1 |$ \pm$| 20
Case 2: moving in (⁠|$-$| 0.76, |$-$| 1.23) [mas yr|$ ^{-1}$| ] with respect
to the system (result of the kinematical model fitting)
|$ V_{R}$| [km s|$ ^{-1}$| ]51 |$ \pm$| 17
|$ V_{\theta}$| [km s|$ ^{-1}$| ]169 |$ \pm$| 22
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 2 |$ \pm$| 20
Case 3: moving in (⁠|$-$| 3, |$-$| 5) [mas yr|$ ^{-1}$| ]
with respect to the system
|$ V_{R}$| [km s|$ ^{-1}$| ]6 |$ \pm$| 13
|$ V_{\theta}$| [km s|$ ^{-1}$| ]228 |$ \pm$| 17
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 7 |$ \pm$| 20
*

Input value for IRAS 18286|$-$| 0959.

†

Input value for the Sun in the Milky Way.

‡

Motion of the Sun with respect to the local standard of rest, cited from Francis and Anderson (2009) (cf., Dehnen & Binney 1998).

§

Height of the Sun from the Galactic mid-plane, cited from Hammersley et al. (1995).

Table 5
Open in new tab

Location and 3D motion of IRAS 18286|$-$|0959 in the Milky Way estimated from the VERA astrometry.

ParameterValue
Galactic coordinates, (⁠|$ l$| , |$ b$| ) [|$ ^{\circ}$| ]*(21.80, |$-$| 0.13)
Heliocentric distance, |$ D$| [kpc]*3.61 |$ \pm$| 0.63
Systemic LSR velocity, |$ V_{\rm sys}$| [km s|$ ^{-1}$| ]*60 |$ \pm$| 5
|$ R_{\rm0}$| [kpc]†8.0
|$ \Theta_{\rm0}$| [km s|$ ^{-1}$| ]†220
(⁠|$ U_{\odot}$| , |$ V_{\odot}$| , |$ W_{\odot}$| ) [km s|$ ^{-1}$| ]‡(7.5, 13.5, 6.8)
|$ z_{\rm0}$| [pc]§16
|$ R_{\rm gal}$| [kpc]4.84 |$ \pm$| 0.50
|$ z$| [pc]7 |$ \pm$| 1
Case 1: fixed in the system
|$ V_{R}$| [km s|$ ^{-1}$| ]66 |$ \pm$| 19
|$ V_{\theta}$| [km s|$ ^{-1}$| ]148 |$ \pm$| 25
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 1 |$ \pm$| 20
Case 2: moving in (⁠|$-$| 0.76, |$-$| 1.23) [mas yr|$ ^{-1}$| ] with respect
to the system (result of the kinematical model fitting)
|$ V_{R}$| [km s|$ ^{-1}$| ]51 |$ \pm$| 17
|$ V_{\theta}$| [km s|$ ^{-1}$| ]169 |$ \pm$| 22
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 2 |$ \pm$| 20
Case 3: moving in (⁠|$-$| 3, |$-$| 5) [mas yr|$ ^{-1}$| ]
with respect to the system
|$ V_{R}$| [km s|$ ^{-1}$| ]6 |$ \pm$| 13
|$ V_{\theta}$| [km s|$ ^{-1}$| ]228 |$ \pm$| 17
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 7 |$ \pm$| 20
ParameterValue
Galactic coordinates, (⁠|$ l$| , |$ b$| ) [|$ ^{\circ}$| ]*(21.80, |$-$| 0.13)
Heliocentric distance, |$ D$| [kpc]*3.61 |$ \pm$| 0.63
Systemic LSR velocity, |$ V_{\rm sys}$| [km s|$ ^{-1}$| ]*60 |$ \pm$| 5
|$ R_{\rm0}$| [kpc]†8.0
|$ \Theta_{\rm0}$| [km s|$ ^{-1}$| ]†220
(⁠|$ U_{\odot}$| , |$ V_{\odot}$| , |$ W_{\odot}$| ) [km s|$ ^{-1}$| ]‡(7.5, 13.5, 6.8)
|$ z_{\rm0}$| [pc]§16
|$ R_{\rm gal}$| [kpc]4.84 |$ \pm$| 0.50
|$ z$| [pc]7 |$ \pm$| 1
Case 1: fixed in the system
|$ V_{R}$| [km s|$ ^{-1}$| ]66 |$ \pm$| 19
|$ V_{\theta}$| [km s|$ ^{-1}$| ]148 |$ \pm$| 25
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 1 |$ \pm$| 20
Case 2: moving in (⁠|$-$| 0.76, |$-$| 1.23) [mas yr|$ ^{-1}$| ] with respect
to the system (result of the kinematical model fitting)
|$ V_{R}$| [km s|$ ^{-1}$| ]51 |$ \pm$| 17
|$ V_{\theta}$| [km s|$ ^{-1}$| ]169 |$ \pm$| 22
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 2 |$ \pm$| 20
Case 3: moving in (⁠|$-$| 3, |$-$| 5) [mas yr|$ ^{-1}$| ]
with respect to the system
|$ V_{R}$| [km s|$ ^{-1}$| ]6 |$ \pm$| 13
|$ V_{\theta}$| [km s|$ ^{-1}$| ]228 |$ \pm$| 17
|$ V_{z}$| [km s|$ ^{-1}$| ]|$-$| 7 |$ \pm$| 20
*

Input value for IRAS 18286|$-$| 0959.

†

Input value for the Sun in the Milky Way.

‡

Motion of the Sun with respect to the local standard of rest, cited from Francis and Anderson (2009) (cf., Dehnen & Binney 1998).

§

Height of the Sun from the Galactic mid-plane, cited from Hammersley et al. (1995).

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