TYC 3980-1081-1 having a V magnitude of 10.5, is the closest confirmed star in this sample at 6.46pc ({pi}=154.8+/-12.1mas, pmra=-21.0+/-13.6mas/yr, pmdc=149.5+/-13.7mas/yr), making this the 97th nearest star system to the Sun. The new URAT parallax is slightly farther than the photometrically estimated distance of 5.9pc from the UCAC4 nearby star survey paper (Finch et al. 2014, cat. J/AJ/148/119). This star shows no signs of an elongated or blended image and no issues are seen with the fit solution. Our measurements suggest that this would be the 97th closest star system according to the RECONS (www.recons.org) 100 nearest star systems.
UPM0012+5215    having a URAT magnitude of 15.62, is the third closest new discovery in this sample at 6.48pc ({pi}=154.3+/-17.3mas, pmra=42.6+/-14.5mas/yr, pmdc=46.2+/-14.0mas/yr). Our measurements suggest that this would be the 99th nearest star system to the Sun. The sky image of this star did show a blended image and has been noted as suspect in Table4, indicating that the solution may be erroneous.
UPM2340+4625    having a URAT magnitude of 14.93, is the second closest new discovery in this sample at 4.8pc ({pi}=206.5+/-17.3mas, pmra=48.5+/-12.3mas/yr, pmdc=42.0+/-12.0mas/yr). Our measurements suggest that this would be the 44th nearest star system to the Sun. The sky image of this star does show an elongated image and the solution has been noted as suspect in Table4. However, this star shares a large parallax with UPM 2340+4631 (within 2{sigma} of each other) at a separation less than 7 arcmin away, indicating that it may be a binary. The sky image of UPM 2340+4631 does show an elongated image and has been noted as suspect in Table4, indicating that the solution may be erroneous.
UPM0429+3806    having a URAT magnitude of 15.36, is the closest new discovery in this sample at 4.4pc ({pi}=227.2+/-19.0mas, pmra=114.7+/-14.0mas/yr, pmdc=3.8+/-13.0mas/yr). Our measurements suggest that this would be the 34th nearest star system to the Sun. The sky image of this star did show an elongated image and has been noted as suspect in Table4, indicating that the solution may be erroneous.
UPM1758-0058    UPM 1758-0058, UPM 1758-0057, UPM 1758-0055, and UPM 1758-0055 all share a large parallax ({pi}=103.2+/-18.4mas, 110.6+/-18.9mas, 103.5+/-22.0mas, 109.5+/-23.3mas) within 1{sigma}, respectively, at a separation less than 12 arcmin on the sky and all with small proper motions. None of the sky images for these stars have been tagged as having a blended or elongated image. However, these stars have been tagged as suspect in Table4 due to scatter seen in the fits, indicating that the solutions may be erroneous.
UPM1758-0057    UPM 1758-0058, UPM 1758-0057, UPM 1758-0055, and UPM 1758-0055 all share a large parallax ({pi}=103.2+/-18.4mas, 110.6+/-18.9mas, 103.5+/-22.0mas, 109.5+/-23.3mas) within 1{sigma}, respectively, at a separation less than 12 arcmin on the sky and all with small proper motions. None of the sky images for these stars have been tagged as having a blended or elongated image. However, these stars have been tagged as suspect in Table4 due to scatter seen in the fits, indicating that the solutions may be erroneous.
UPM1758-0055    UPM 1758-0058, UPM 1758-0057, UPM 1758-0055, and UPM 1758-0055 all share a large parallax ({pi}=103.2+/-18.4mas, 110.6+/-18.9mas, 103.5+/-22.0mas, 109.5+/-23.3mas) within 1{sigma}, respectively, at a separation less than 12 arcmin on the sky and all with small proper motions. None of the sky images for these stars have been tagged as having a blended or elongated image. However, these stars have been tagged as suspect in Table4 due to scatter seen in the fits, indicating that the solutions may be erroneous.